Basaltic volcanism on the eucrite parent body - Petrology and chemistry of the polymict eucrite ALHA80102

NASA Technical Reports Server (NTRS)

Treiman, A. H.; Drake, M. J.

1985-01-01

The polymict eucrite meteorite ALHA80102 is an unequilibrated breccia of basaltic and gabbroic clasts in a fragmental matrix. Clasts include basalts of many textural types, cumulate gabbro, black 'glass', and ferroan troctolite (plagioclase, silica, Fe-rich olivine, ilmenite, mesostasis). Ferroan troctolite has not been previously reported from eucrites or howardites; it is interpreted as the end-product of fractional crystallization of eucritic magmas. Bulk and trace element compositions (by electron microprobe and INAA) of clasts and matrix from ALHA80102 are similar to those of other eucrites; the meteorite contains clasts similar to Juvinas and to Stannern. A clast of cumulate eucrite gabbro is enriched in the light rare earths (La/Lu = 2XCI). This clast is interpreted as an unrepresentative sample of metamorphically equilibrated gabbro; LREE-enriched magmas need not be invoked. ALHA80102 is similar to other polymict eucrites from the Allan Hills and may be paired with ALHA76005, ALHA77302, and ALHA78040.

Petrology of eucrites, howardites and mesosiderites

USGS Publications Warehouse

Duke, M.B.; Silver, L.T.

1967-01-01

The eucrite and howardite calcium-rich achondrites and many mesosiderites are considered as a coherent meteorite assemblage, their silicates consisting essentially of calciumpoor monoclinic and orthorhombic pyroxenes and calcium-rich plagioclase feldspar. The achondrites can be grouped according to their brecciated structure as follows: eucrites-unbrecciated and monomict brecciated achondrites; howardites-polymict brecciated achondrites. Many mesosiderites contain brecciated structures; they are distinguished from the achondrites by their large metallic fraction. The structure and composition of rock fragments in the breccias indicate a complicated sequence of events including magmatic differentiation, brecciation, recrystallization and refragmentation, and ejection from the parent body. Detailed mineralogical and chemical data suggest that the magmatic differentiation proceeded primarily by the separation of pyroxene from an ultrabasic parent material that had a much lower alkali content than ordinary chondrites. Magmatic crystallization took place in environments ranging from extrusive to deep-seated intrusive. Polymict breccias contain fragments with a wide variety of magmatic and recrystallization textures, which suggests that the breccias were formed either in very large or repeated fragmentation events. Monomict breccias contain fragments with a small range of similar magmatic textures, which suggests that these breccias were formed by small or single events. Petrographic evidence suggests that many of the breccias are impact breccias. Either in their original magmatic crystallization sites or in the sites of breccia accumulation, most of these meteorites apparently had a near-surface location prior to ejection from the parent body. Evidence obtained from eucrites, howardites and mesosiderites forms an important part of our understanding of the early evolution of the surface regions of their parent body. Chemical and oxidation conditions were different from those presently found in the Earth's crust and upper mantle, but the necessary conditions may have been present in the early history of the Earth. A lunar origin for eucrites, howardites and mesosiderites is proposed, but an asteroidal origin can not be presently excluded. ?? 1967.

Chemical zoning and homogenization of Pasamonte-type pyroxene and their bearing on thermal metamorphism of a howardite parent body

NASA Technical Reports Server (NTRS)

Miyamoto, M.; Duke, M. B.; Mckay, D. S.

1985-01-01

The Mg-Fe zoning of pyroxenes in Pasamonte and Juvinas eucrites is examined in order to gain a better understanding of the metamorphism in the surface layer of a eucrite/howardite parent body. Three distinct types of Ca-Mg-Fe zoning of Pasamonte pyroxenes are identified. The wide compositional range of the zoned pyroxenes suggests that Pasamonte is less metamorphosed than previously believed. It is also found that a Pasamonte-type pyroxene may yield a Juvinas-type pyroxene by thermal metamorphism. Calculations imply that the homogenization of Juvinas pyroxenes may have occurred during later reheating events rather than during initial cooling.

Core Formation and Evolution of Asteroid 4 Vesta

NASA Technical Reports Server (NTRS)

Kiefer, Walter S.; Mittlefehldt, David W.

2014-01-01

The howardites, eucrites, and diogenites (HEDs) are a suite of related meteorite types that formed by igneous and impact processes on the same parent body. Multiple lines of evidence, including infrared spectroscopy of the asteroid belt and the petrology and geochemistry of the HEDs, suggest that the asteroid 4 Vesta is the parent body for the HEDs. Observations by NASA's Dawn spacecraft mission strongly support the conclusion that the HEDs are from Vesta. The abundances of the moderately siderophile elements Ni, Co, Mo, W, and P in eucrites require that most or all of the metallic phase in Vesta segregated to form a core prior to eucrite solidification. These observations place important constraints on the mode and timescale of core formation on Vesta. Possible core formation mechanisms include porous flow, which potentially could occur prior to initiation of silicate melting, and metallic rain in a largely molten silicate magma ocean. Once the core forms, convection within the core could possible sustain a magnetic dynamo for a period of time. We consider each process in turn.

Electrochemical measurements and thermodynamic calculations of redox equilibria in pallasite meteorites - Implications for the eucrite parent body

NASA Technical Reports Server (NTRS)

Righter, Kevin; Arculus, Richard J.; Paslick, Cassi; Delano, John W.

1990-01-01

The intrinsic oxygen fugacity (IOF) of olivine separates from the Salta, Springwater, and Eagle Station pallasites was measured between 850 and 1150 C using oxygen-specific solid zirconia electrolytes at 100,000 Pa. Thermodynamic calculations of redox equilibria involving equalibrium pallasite assemblages are in good agreement with the experimental results and provide a lower limit to pallasite redox stability; others involving disequilibrium assemblages, suggest that pallasites experienced localized, late-stage oxidation and reduction effects. Consideration of the redox buffer metal-olivine-orthopyroxene utilizing calculated Eucrite Parent Body (EPB) mantle phase compositions indicates that small redox gradients may have existed in the EPB. Such gradients may have produced strong compositional variation within the EPB. In addition, there is apparently significant redox heterogeneity in the source area of Eagle Station Trio pallasites and Bocaiuva iron meteorites.

Pyroxene Homogenization and the Isotopic Systematics of Eucrites

NASA Technical Reports Server (NTRS)

Nyquist, L. E.; Bogard, D. D.

1996-01-01

The original Mg-Fe zoning of eucritic pyroxenes has in nearly all cases been partly homogenized, an observation that has been combined with other petrographic and compositional criteria to establish a scale of thermal "metamorphism" for eucrites. To evaluate hypotheses explaining development of conditions on the HED parent body (Vesta?) leading to pyroxene homogenization against their chronological implications, it is necessary to know whether pyroxene metamorphism was recorded in the isotopic systems. However, identifying the effects of the thermal metamorphism with specific effects in the isotopic systems has been difficult, due in part to a lack of correlated isotopic and mineralogical studies of the same eucrites. Furthermore, isotopic studies often place high demands on analytical capabilities, resulting in slow growth of the isotopic database. Additionally, some isotopic systems would not respond in a direct and sensitive way to pyroxene homogenization. Nevertheless, sufficient data exist to generalize some observations, and to identify directions of potentially fruitful investigations.

A numerical treatment of melt/solid segregation - Size of the eucrite parent body and stability of the terrestrial low-velocity zone

NASA Technical Reports Server (NTRS)

Walker, D.; Stolper, E. M.; Hays, J. F.

1978-01-01

Crystal sinking to form cumulates and melt percolation toward segregation in magma pools can be treated with modifications of Stokes' and Darcy's laws, respectively. The velocity of crystals and melt depends, among other things, on the force of gravity (g) driving the separations and the cooling time of the environment. The increase of g promotes more efficient differentiation, whereas the increase of cooling rate limits the extent to which crystals and liquid can separate. The rate at which separation occurs is strongly dependent on the proportion of liquid that is present. The observation of cumulates and segregated melts among the eucrite meteorites is used as a basis for calculating the g (and planet size) required to perform these differentiations. The eucrite parent body was probably at least 10-100 km in radius. The earth's low velocity zone (LVZ) is shown to be unstable with respect to draining itself of excess melt if the melt forms an interconnecting network. A geologically persistent LVZ with a homogeneous distribution of melt can be maintained with melt fractions only on the order of 0.1% or less.

Petrology of Igneous Clasts in Regolithic Howardite EET 87503

NASA Technical Reports Server (NTRS)

Hodges, Z. V.; Mittlefehldt, D. W.

2017-01-01

The howardite, eucrite and diogenite (HED) clan of meteorites is widely considered to originate from asteroid 4 Vesta, as a result of a global magma ocean style of differentiation. A global magmatic stage would allow silicate material to be well mixed, destroying any initial heterogeneity that may have been present resulting in the uniformity of eucrite and diogenite delta(exp 17)O, for example. The Fe/Mn ratio of mafic phases in planetary basalts can be diagnostic of different source bodies as this ratio is little-affected by igneous processes, so long as the oxygen and sulphur fugacities are buffered. Here, pyroxene Fe/Mn ratios in mafic clasts in howardite EET 87503 have been determined to further evaluate whether the HED parent asteroid is uniform. Uniformity would suggest that the parent asteroid was subject to homogenization prior to the formation of HED lithologies, likely through an extensive melting phase. Whereas, distinct differences may point towards heterogeneity of the parent body.

The asteroid-meteorite connection: Forging a new link to Vesta as the parent body of basaltic achondrite (HED) meteorites

NASA Technical Reports Server (NTRS)

Binzel, R. P.

1993-01-01

Asteroid 4 Vesta has been at the center of the debate over the identity of the howardite eucrite diogenite (HED) parent body since the early 1970s. Despite its unique (among the 500 largest asteroids) compositional match to HED meteorites, substantial dynamical difficulties in delivering fragments from Vesta to the Earth have precluded any conclusive HED parent body link. These dynamical difficulties arise because Vesta's orbital location is far from known resonances. Consequently, it has been argued as dynamically improbable that meteoroid-sized (1 km) fragments could be excavated from Vesta with sufficient velocities to reach the resonances. Through new astronomical observations, numerous small (4-7 km) asteroids between Vesta and the 3:1 resonance have been discovered to have eucrite and diogenite compositions. Based on similar orbital elements to Vesta, all of these new asteroids are likely large impact fragments excavated from Vesta. Their current orbits imply ejection velocities in excess of 700 m/sec. Smaller (1 km) fragments can therefore be expected to have been ejected with velocities greater than 1 km/sec, sufficient to reach the 3:1 and v6 resonances. Thus it now appears to be dynamically viable for Vesta to be linked as the HED parent body.

Experimental investigation of the partitioning of phosphorus between metal and silicate phases - Implications for the earth, moon and eucrite parent body

NASA Technical Reports Server (NTRS)

Newsom, H. E.; Drake, M. J.

1983-01-01

An experimental study is reported of the partitioning of Phosphorus between solid metal and basaltic silicate liquid as a function of temperature and oxygen fugacity and of the implications for the earth, moon and eucrite parent body (EPB). The relationship established between the partition coefficient and the fugacity is given at 1190 C by log D(P) = -1.12 log fO2 - 15.95 and by log D(P) = -1.53 log fO2 17.73 at 1300 C. The partition coefficient D(P) was determined, and it is found to be consistent with a valence state of 5 for P in the molten silicate. Using the determined coefficient the low P/La ratios of the earth, moon, and eucrites relative to C1 chondrites can be explained. The lowering of the P/La ratio in the eucrites relative to Cl chondrite by a factor of 40 can be explained by partitioning P into 20-25 wt% sulfur-bearing metallic liquid corresponding to 5-25% of the total metal plus silicate system. The low P/La and W/La ratios in the moon may be explained by the partitioning of P and W into metal during formation of a small core by separation of liquid metal from silicate at low degrees of partial melting of the silicates. These observations are consistent with independent formation of the moon and the earth.

Serra Pelada: the first Amazonian Meteorite fall is a Eucrite (basalt) from Asteroid 4-Vesta.

PubMed

Zucolotto, Maria Elizabeth; Tosi, Amanda A; Villaça, Caio V N; Moutinho, André L R; Andrade, Diana P P; Faulstich, Fabiano; Gomes, Angelo M S; Rios, Debora C; Rocha, Marcilio C

2018-01-01

Serra Pelada is the newest Brazilian eucrite and the first recovered fall from Amazonia (State of Pará, Brazil, June 29th 2017). In this paper, we report on its petrography, chemistry, mineralogy and its magnetic properties. Study of four thin sections reveals that the meteorite is brecciated, containing basaltic and gabbroic clasts, as well of recrystallized impact melt, embedded into a fine-medium grained matrix. Chemical analyses suggest that Serra Pelada is a monomict basaltic eucritic breccia, and that the meteorite is a normal member of the HED suite. Our results provide additional geological and compositional information on the lithological diversity of its parent body. The mineralogy of Serra Pelada consists basically of low-Ca pyroxene and high-Ca plagioclase with accessory minerals such as quartz, sulphide (troilite), chromite - ulvöspinel and ilmenite. These data are consistent with the meteorite being an eucrite, a basaltic achondrite and a member of the howardite-eucrite-diogenite (HED) clan of meteorites which most likely are from the crust asteroid 4 Vesta.

Effects of Varying Proportions of Glass on Reflectance Spectra of HED Polymict Breccias

NASA Technical Reports Server (NTRS)

Buchanan, P. C.; Reddy, V; LeCorre, L.; Cloutis, E. A.; Mann, P.; Le, L.

2014-01-01

Some meteorites contain significant amounts of glass, which, in most cases, probably results from impact processes on parent bodies.. Yamato 82202 is an example of one of the unequilibrated eucrites that contains significant proportions of impact glass distributed as veins throughout the meteorite. In other cases, fragments of glass are distributed throughout polymict breccias. For example, the polymict eucrite EET 87509 contains rare angular fragments of devitrified glass. Proportions of glass in most of these meteorites and in lithic clasts within these meteorites may vary locally from small amounts (less than one percent) to much larger amounts (subequal proportions of glass and mineral material). For example, some fragments within the South African polymict eucrite Macibini contain approximately 50% glass. The presence of these variable proportions of meteorite glass confirm the increased recognition that impact processes played an important role in the histories of asteroidal bodies. This study attempts to quantify the effects of a glass component on reflectance spectra by analyzing in the laboratory mixtures of varying proportions of a well-characterized HED polymict breccia and glass derived by melting a bulk sample of that breccia.

Impact melting of the Cachari eucrite 3.0 Gy ago

NASA Technical Reports Server (NTRS)

Bogard, D. D.; Taylor, G. J.; Keil, K.; Smith, M. R.; Schmitt, R. A.

1985-01-01

The chemical compositions and Ar-isotope gas-retention ages of host phase and glass veins in the Cachari eucrite are determined by microprobe and neutron-activation analysis and mass spectrometry, respectively. The results are presented in tables, graphs, and back-scattered electron images and characterized in detail. The compositions are found to support the thesis that the glass formed by shock melting of the host rock (or of rock having the same composition). The Ar-39/Ar-40 ages of host and glass are given as 3.04 + or - 0.07 Gyr and 3.47 + or - 0.04 Gyr, respectively; the former value is taken as the true data of melting, and the latter is attributed to incomplete postmelt degassing of Ar from the glass phase. The implications of the relative youth of this and other eucrites and howardites for the regolith history of the parent body are considered.

Chips off of Asteroid 4 Vesta: Evidence for the Parent Body of Basaltic Achondrite Meteorites.

PubMed

Binzel, R P; Xu, S

1993-04-09

For more than two decades, asteroid 4 Vesta has been debated as the source for the eucrite, diogenite, and howardite classes of basaltic achondrite meteorites. Its basaltic achondrite spectral properties are unlike those of other large main-belt asteroids. Telescopic measurements have revealed 20 small (diameters

The mineralogy, petrology, and composition of anomalous eucrite Emmaville

NASA Astrophysics Data System (ADS)

Barrett, T. J.; Mittlefehldt, D. W.; Greenwood, R. C.; Charlier, B. L. A.; Hammond, S. J.; Ross, D. K.; Anand, M.; Franchi, I. A.; Abernethy, F. A. J.; Grady, M. M.

2017-04-01

The Emmaville eucrite is a relatively poorly studied basaltic achondrite with an anomalous oxygen isotope signature. In this study, we report comprehensive mineralogical, petrographic, and geochemical data from Emmaville in order to understand its petrogenesis and relationship with the basaltic eucrites. Emmaville is an unusually fine-grained, hornfelsic-textured metabasalt with pervasive impact melt veins and mineral compositions similar to those of typical basaltic eucrites. The major and trace element bulk composition of Emmaville is also typical of a basaltic eucrite. Three separated individual lithologies were also analyzed for O isotopes; a dark gray fraction (E1), a shocked lithology (E2), and a lighter gray portion (E3). Fractions E1 and E2 shared similar O isotope compositions to the bulk sample (E-B), whereas the lighter gray portion (E3) is slightly elevated in Δ17O and significantly elevated in δ18O compared to bulk. No evidence for any exogenous material is observed in the thin sections, coupled with the striking compositional similarity to typical basaltic eucrites, appears to preclude a simple impact-mixing hypothesis. The O-isotopes of Emmaville are similar to those of Bunburra Rockhole, A-881394, and EET 92023, and thus distinct from the majority of the HEDs, despite having similarities in petrology, mineral, and bulk compositions. It would, therefore, seem plausible that all four of these samples are derived from a single HED-like parent body that is isotopically distinct from that of the HEDs (Vesta) but similar in composition.

Mineralogy of Inverted Pigeonite and Plagioclase in Cumulate Eucrites Y-980433 and Y-980318 with Reference to Early Crust Formation of the Vesta-Like Body

NASA Technical Reports Server (NTRS)

Takeda, H.; Ohtake, M.; Hiroi, T.; Nyquist, L. E.; Shih, C.-Y.; Yamaguchi, A.; Nagaoka, H.

2011-01-01

On July 16, the Dawn spacecraft became the first probe to enter orbit around asteroid 4 Vesta and will study the asteroid for a year before departing for Ceres. The Vesta-HED link is directly tied to the observed and inferred mineralogy of the asteroid and the mineralogy of the meteorites [1]. Pieters et al. [2] reported reflectance spectra of the Yamato- (Y-)980318 cumulate eucrite as a part of their study on the Asteroid-Meteorite Links in connection with the Dawn Mission. Pyroxenes and calcic plagioclase are the dominant minerals present in HED meteorites and provide multiple clues about how the parent body evolved [1]. The differentiation trends of HED meteorites are much simpler than those of the lunar crust

Ibitira: A basaltic achondrite from a distinct parent asteroid

NASA Technical Reports Server (NTRS)

Mittlefehldt, David W.

2004-01-01

I have done detailed petrologic study of Ibitira, nominally classified as a basaltic eucrite. The Fe/Mn ratio of Ibitira pyroxenes with <10 mole % wollastonite component is 36.4 0.4, and is well-resolved from those of five basaltic eucrites studied for comparison; 31.2-32.2. Data for the latter completely overlap. Ibitira pyroxenes have lower Fe/Mg than the basaltic eucrite pyroxenes. Thus, the higher Fe/Mn ratio does not reflect a simple difference in oxidation state. Ibitira also has an oxygen isotopic composition, alkali element contents and a Ti/Hf ratio that distinguish it from basaltic eucrites. These differences support derivation from a distinct parent asteroid. Ibitira is the first recognized representative of the fifth known asteroidal basaltic crust.

Vesta Evolution from Surface Mineralogy: Mafic and Ultramafic Mineral Distribution

NASA Technical Reports Server (NTRS)

DeSanctis, M. C.; Ammannito, E.; Palomba, E.; Longobardo, A.; Mittlefehldt, D. W.; McSween, H. Y; Marchi, S.; Capria, M. T.; Capaccioni, F.; Frigeri, A.;

Could the eucrite Graves Nunataks 98098 be Vesta's equivalent to Lunar KREEP?

NASA Astrophysics Data System (ADS)

Sarafian, A. R.; Marschall, H.; Nielsen, S.

2013-12-01

Basaltic eucrites, members of the HED achondrite clan, are thought to derive from the asteroid 4-Vesta [1]. Most eucrites show little compositional and petrographic variability, thus anomalous eucrite could provide key insights into differentiation processes that operated on Vesta. The eucrite Graves Nunataks (GRA) 98098 is an unbrecciated eucrite with cross cutting white tabular veins consisting of mainly equigranular tridymite and euhedral plagioclase with some pyroxene [2]. In addition, GRA has the second highest modal (volume) abundance of apatite in a eucrite studied thus far. The apatite is associated with the veins [2]. The GRA bulk rock composition is enriched in incompatible elements with concentrations ca. 3-5 times higher than in most basaltic eucrites [3]. Additionally, GRA has 10-20 times more Cl than any other analyzed eucritic apatite [2]. Here we measured the trace-element concentrations of plagioclase and pyroxene by laser ablation ICP-MS and the D/H ratio of the apatites by SIMS. In the domains of GRA cut by veins, the trace elements in plagioclase and pyroxene show an up to 15x enrichment in incompatible elements compared to other basaltic eucrites [4]. Here we report the first D/H measurement of any magmatic material from Vesta. The D/H of apatite in GRA is relatively light compared to vSMOW. Based on the high abundance of incompatible elements in GRA and the high Cl content found in apatites, Sarafian et al. [2] suggested that GRA could be akin to Lunar KREEP (lunar rocks enriched in K, REEs and P). With the additional evidence of enriched incompatible elements in plagioclase and pyroxene and the similarity in D/H compared to KREEP, it is likely that GRA was infiltrated by a late-stage melt enriched in incompatible elements, similar to Lunar KREEP. Further study is needed to determine if this late-stage melt formed in a similar manner as KREEP. 1. Consolmango, G.J. and M.J. Drake, Composition and evolution of the eucrite parent body: Evidence from rare earth elements. Geochimica et Cosmochimica Acta, 1977. 41: p. 1271-1282. 2. Sarafian, A.R., M.F. Roden, and A.E. Patiño Douce, The nature of volatiles in eucrites: Clues from apatite. Meteoritics and Planetary Science, 2013. in press. 3. Mittlefehldt, D.W. and M.M. Lindstrom, Geochemistry of eucrites: genesis of basaltic eucrites, and Hf and Ta as petrogenetic indicators for altered antarctic eucrites. Geochimica et Cosmochimica Acta, 2003. 67(10): p. 1911-1934. 4. Hsu, W. and G. Crozaz, Mineral chemistry and the petrogenesis of eucrites: I. Noncumulate eucrites. Geochimica et Cosmochimica Acta, 1996. 60(22): p. 4571-4591.

The Bombardment History of 4 Vesta as Told by Sample Geochronology

NASA Technical Reports Server (NTRS)

Cohen, B. A.

2014-01-01

The Dawn mission showed asteroid 4 Vesta to be an extensively cratered body, ancient in age, with craters in a variety of morphologies and preservation states [1-3]. Tying Vesta's relative crater ages to an absolute impact history can be accomplished through investigations of the HED (howardite, eucrite, diogenite) meteorites. Eucrites are crustal basalts and gabbros, diogenites are mostly orthopyroxenites representing lower crust or upper mantle materials, and howardites are mixed breccias containing both lithologies. Eucrite 53Mn-53Cr systematics show that the HED parent body globally differentiated by 4.56 Ga and fully crystallized soon afterwards [4]. Much later, many eucrites were brecciated and heated by large impacts into the parent body surface. Disturbance ages in eucrites show that multiple large impacts occurred within 1 Gyr after crystallization, showing a history that largely resembles that of the Moon [5-7]. Dawn images also showed that Vesta is covered with a well-developed regolith that is spectrally similar to howardite meteorites [8]. Howardites are polymict regolith breccias made up mostly of clasts of eucrites and diogenites, but which also contain clasts formed by melting of the regolith by relatively large, energetic impact events. Impact-melt clast ages from howardites extend our knowledge of the impact history of Vesta, expanding on eucrite disturbance ages and helping give absolute age context to the observed crater-counts produced using Dawn data. The distribution of 40Ar-39Ar ages of impact-melt clasts in howardites shows that they formed within the time period 3.3-3.8 Ga [9]. These, and other impact-melted HED materials, have distinct age and compositional characteristics that suggest they formed in discrete impact events. In order to create these crystalline impact-melt products on the surface of Vesta, the impacts during this time period must have had velocities much higher than 5 km/s, the main belt average [10]. This is inconsistent with formation by a normal distribution of impact velocities and points instead to a unique period where high-velocity collisions were more frequent than currently observed. Until now, impact-reset ages in the HED meteorites have been be interpreted under the umbrella of the canonical lunar cataclysm where an increase in the absolute number of bombarding objects is responsible for creating larger absolute amounts of impact-affected and impact-melted rocks, statistically increasing their chances of being found on Earth and dated. However, the distribution of age among the howardite impact-melt clasts may not necessarily result from an increased number of impacts, but rather result from impacts of higher velocity. The changeover from a typical main belt velocity profile to this regime of increased velocity population at Vesta occurs contemporaneously with a similar transition at the Moon, indicating that howardite impact-melt clast ages reinforce the notion of a dynamically unusual episode of bombardment in the inner solar system beginning at around 4.0 Ga.

The Dos and Don'ts of how to Build a Planet, Using the Moon as an Example

NASA Technical Reports Server (NTRS)

Jones, J. H.

2006-01-01

The bulk chemical compositions of planets may yield important clues concerning planetary origins. Failing that, bulk compositions are still important, in that they constrain calculation of planetary mineralogies and also constrain the petrogenesis of basaltic magmas. In the case of the Earth, there is little or no debate about the composition of the Earth's upper mantle. This is because our sample collections contain peridotitic xenoliths of that mantle. The most fertile of these are believed to have been little modified from their primary compositions. Using these samples and chondritic meteorites as a starting point, small perturbations on the compositions of existing samples allow useful reconstruction of the bulk silicate Earth (BSE). Elsewhere, I have argued that the next simplest case is the Eucrite Parent Body (EPB). Reconstructions based on Sc partitioning indicate that the EPB can be well approximated by a mixture of 20% eucrite and 80% equilibrium olivine. This leads to a parent body that is similar to CO (or devolatilized CM) chondrites. Partial melting experiments on CM chondrites confirm this model, because the residual solids in these experiments are dominated by olivine with minor pigonite [3]. The most difficult bodies to reconstruct are those that have undergone the most differentiation. Both the Moon and Mars may have passed through a magma ocean stage. In any event, lunar and martian basalts, unlike eucrites, were not derived from undifferentiated source regions. Reconstructions are primarily based on compositional trends within the basalts themselves with some critical assumptions: (i) Refractory lithophile elements (Ca, Al, REE, actinides) are presumed to be in chondritic relative abundances; and (ii) some major element ratio is believed to exist in a chondritic ratio (e.g., Mg/Si, Mg/Al). The most commonly used parameter is Mg/Si.

Further Evidence for Geochemical Diversity, and Possible Bimodality, Among Cumulate Eucrites

NASA Astrophysics Data System (ADS)

Warren, P. H.; Kallemeyn, G. W.

1992-07-01

We have used INAA, RNAA, and fused-bead analysis to determine the bulk compositions of numerous Antarctic eucrites (and also the LEW88516 SNC meteorite). Only a few of the most unusual eucrites can be discussed in the limited space here. Takeda et al. (1988) noted that Y791195 is a slowly cooled eucrite, with an equant, medium-grained texture, and pyroxene exsolution lamellae up to 10 micrometers across. In Y791195,81-3, we find lamellae up to 14 micrometers across. In this respect, Y791195 resembles RKPA80224, in which exsolution lamellae up to 12 micrometers across. We have previously discussed the evidence that RKPA80224 is a mildly accumulative rock that formed from an unusually low-mg parent melt. Our second analysis of RKPA80224 only partly confirms the unusually low incompatible trace element (ITE) content, but the Ce anomaly is consistently small (Ce/La = 0.90-1.02 x CI), and based on a weighted mean composition the implied parent melt is still unlike any noncumulate eucrite (see Fig. 1, which shows results from mass balance calculations modeling the sample as a mixture of cumulus px and plag, plus trapped melt). A parent melt similar to an extreme low-mg, variant of the "Nuevo Laredo Trend" would plausibly account for RKPA80224. The spectrum of possible parents for Y791195 is similar, even though its "true" Sm content is slightly obscured by weathering (Ce/La = 1.4 x CI). The [Sm] used in the figure is scaled to the highest CI-normalized REE concentration. Data of Mittlefehldt and Lindstrom (1991) indicate that except for exterior samples "showing extreme rustiness," Sm even in weathered eucrites is generally not altered beyond a few tens of pct. relative (sample size seems to account for more of the variation in [Sm] among interior, non-rusty samples). Even assuming a Sm content twice that assumed in the figure, the parent melt still must be well to the low-MgO/FeO, low-Sm side of all known eucrites. The LEW87002 eucrite is brecciated, but probably monomict. The pyroxene is uniformly Mg-rich (opx mg = 68), yet diogenitic px is not present. No Ce anomaly was detected. If lunar standards can be applied to eucrites, our RNAA siderophile result for Au gives a marginal indication of "pristinity": [Au] = 2.5 X 10^-4 times CI; also [Re] = 4.3 X 10^-4 times CI, but [Ir] = 7.4 X 10^-4 times CI (possibly linked to the unusually mafic nature of this rock). Like Binda and the mildly accumulative Pomozdino, LEW87002 appears to be the product of a melt along the moderate-mg, high- ITE "Stannem Trend." Collectively, these samples suggest that cumulate eucrites formed from parent melts more diverse than the known noncumulate eucrites. The data also hint at a geochemical bimodality for the parent melts, reminiscent of the bimodality among ancient lunar cumulates, which show a paradoxical tendency for high-mg cumulates to be more ITE-rich than low-mg cumulates. The same basic mechanism might be responsible: later melts are more directly linked to the high-mg mantle, but tend to be contaminated by mixing with residual melts left over from the slightly older Nuevo Laredo Trend linked cumulates. References: Delaney J. S. (1988) Lunar and Planet. Sci. XX, 236-237. Mittlefehldt D. W. and Lindstrom M. M. (1991) Geochim. Cosmochim. Acta 55, 77-87. Takeda H., Tagai T., and Graham A. (1988) Thirteenth Symp. Ant. Mets. (Tokyo), pp. 142-144. Figure 1, which in the hard copy appears here, shows cumulate and cumulate-like eucrites and possible parent melt compositions.

Dawn at Vesta: testing the protoplanetary paradigm

USGS Publications Warehouse

Russell, C.T.; Raymond, C.A.; Coradini, A.; McSween, H.Y.; Zuber, M.T.; Nathues, A.; DeSanctis, Maria-Cristina; Jaumann, R.; Konopliv, A.S.; Preusker, F.; Asmar, S.W.; Park, R.S.; Gaskell, R.; Keller, H.U.; Mottola, S.; Roatsch, T.; Scully, J.E.C.; Smith, D.E.; Tricarico, P.; Toplis, M.J.; Christensen, U.R.; Feldman, W.C.; Lawrence, D.J.; McCoy, T.J.; Prettyman, T.H.; Reedy, R.C.; Sykes, M.E.; Titus, T.N.

2012-01-01

The Dawn spacecraft targeted 4 Vesta, believed to be a remnant intact protoplanet from the earliest epoch of solar system formation, based on analyses of howardite-eucrite-diogenite (HED) meteorites that indicate a differentiated parent body. Dawn observations reveal a giant basin at Vesta's south pole, whose excavation was sufficient to produce Vesta-family asteroids (Vestoids) and HED meteorites. The spatially resolved mineralogy of the surface reflects the composition of the HED meteorites, confirming the formation of Vesta's crust by melting of a chondritic parent body. Vesta's mass, volume, and gravitational field are consistent with a core having an average radius of 107 to 113 kilometers, indicating sufficient internal melting to segregate iron. Dawn's results confirm predictions that Vesta differentiated and support its identification as the parent body of the HEDs.

Petrology of Anomalous Mafic Achondrite Polymict Breccia Pasamonte

NASA Technical Reports Server (NTRS)

Mittlefehldt, D. W.; Berger, E. L.; Le, L.

2017-01-01

The most common asteroidal igneous meteorites are eucrite-type basalts and gabbros - rocks composed of ferroan pigeonite and augite, calcic plagioclase, silica, ilmenite, troilite, Ca-phosphate, chromite and Fe-metal [1]. These rocks are thought to have formed on a single asteroid, widely considered to be 4 Vesta, along with howardites and diogenites [1, 2]. High precision O-isotopic analyses have shown that some eucrites have small, well-resolved O-isotopic differences from the group mean [3-5]. These Oanomalous eucrites are thought to hail from asteroidal parents that are distinct from that of eucrites [5]. Three O-anomalous eucrites are PCA 82502, PCA 91007 (paired) and Pasamonte, all of which have the same O-isotopic composition [5, 6]. Our petrologic studies have shown that PCA 82502 and PCA 91007 have well-resolved anomalies in low-Ca pyroxene Fe/Mn compared to eucrites [6]. Divalent Mn and Fe are homologous species that do not greatly fractionate during igneous processes; mafic mineral Fe/Mn can be used to fingerprint parent object sources [7]. Previous petrological studies of Pasamonte [8-10] have not yielded sufficiently precise Fe/Mn ratios to allow distinction of anomalies of the scale of those found for the PCA basalts. We have begun petrological study of Pasamonte for comparison with our results on normal and anomalous eucrites [6], and to constrain its origin.

Planetary basalts - Chemistry and petrology

NASA Technical Reports Server (NTRS)

Papike, J. J.; Bence, A. E.

1979-01-01

Recent literature (1975-1978) on planetary basalts is reviewed. Terrestrial basalts are considered in relation to Nd and Sm isotopic studies, magma mixing, chemical and mineralogical heterogeneities in basalt source regions, and partial melting controls on basalt chemistry. Attention is also given to features of mare basalts, eucrites, and comparisons of basalts for the earth, the moon, and the parent body of basaltic achondrites.

Petrologic and Chemical Characterization of a Suite of Antarctic Diogenites

NASA Technical Reports Server (NTRS)

Mittlefehldt, D. W.; Mertzman, S. A.; Peng, Z. X.; Mertzman, K. R.

2013-01-01

The origin of diogenites, ultramafic cumulates related to eucrites, is an unresolved problem [1]. Most diogenites are orthopyroxenites, a few are harzburgites [2], and some are transitional to cumulate eucrites [1, 3]. Cumulate eucrites are gabbros formed by crystal fractionation from basaltic eucrites [4]. The consensus view is that basaltic eucrites are residual melts from global-magma-ocean crystallization on their parent asteroid [4] which is plausibly Vesta [5]. However, the petrologic and compositional characteristics of diogenites seem to preclude a magma ocean origin [1, 4]. We are doing a petrologic and chemical study of new or unusual diogenites with the ultimate goals of constraining their genesis, and the geologic evolution of Vesta.

The formation of jupiter, the jovian early bombardment and the delivery of water to the asteroid belt: the case of (4) vesta.

PubMed

Turrini, Diego; Svetsov, Vladimir

2014-01-28

The asteroid (4) Vesta, parent body of the Howardite-Eucrite-Diogenite meteorites, is one of the first bodies that formed, mostly from volatile-depleted material, in the Solar System. The Dawn mission recently provided evidence that hydrated material was delivered to Vesta, possibly in a continuous way, over the last 4 Ga, while the study of the eucritic meteorites revealed a few samples that crystallized in presence of water and volatile elements. The formation of Jupiter and probably its migration occurred in the period when eucrites crystallized, and triggered a phase of bombardment that caused icy planetesimals to cross the asteroid belt. In this work, we study the flux of icy planetesimals on Vesta during the Jovian Early Bombardment and, using hydrodynamic simulations, the outcome of their collisions with the asteroid. We explore how the migration of the giant planet would affect the delivery of water and volatile materials to the asteroid and we discuss our results in the context of the geophysical and collisional evolution of Vesta. In particular, we argue that the observational data are best reproduced if the bulk of the impactors was represented by 1-2 km wide planetesimals and if Jupiter underwent a limited (a fraction of au) displacement.

Bunburra Rockhole: Exploring the Geology of a New Differentiated Basaltic Asteroid

NASA Technical Reports Server (NTRS)

Benedix, G.K.; Bland, P. A.; Friedrich, J. M.; Mittlefehldt, D.; Sanborn, M. E.; Yin, Q.-Z.; Greenwood, R. C; Franchi, L. A.; Bevan, A. W. R.; Towner, M. C.;

The Formation of Jupiter, the Jovian Early Bombardment and the Delivery of Water to the Asteroid Belt: The Case of (4) Vesta

PubMed Central

Turrini, Diego; Svetsov, Vladimir

2014-01-01

The asteroid (4) Vesta, parent body of the Howardite-Eucrite-Diogenite meteorites, is one of the first bodies that formed, mostly from volatile-depleted material, in the Solar System. The Dawn mission recently provided evidence that hydrated material was delivered to Vesta, possibly in a continuous way, over the last 4 Ga, while the study of the eucritic meteorites revealed a few samples that crystallized in presence of water and volatile elements. The formation of Jupiter and probably its migration occurred in the period when eucrites crystallized, and triggered a phase of bombardment that caused icy planetesimals to cross the asteroid belt. In this work, we study the flux of icy planetesimals on Vesta during the Jovian Early Bombardment and, using hydrodynamic simulations, the outcome of their collisions with the asteroid. We explore how the migration of the giant planet would affect the delivery of water and volatile materials to the asteroid and we discuss our results in the context of the geophysical and collisional evolution of Vesta. In particular, we argue that the observational data are best reproduced if the bulk of the impactors was represented by 1–2 km wide planetesimals and if Jupiter underwent a limited (a fraction of au) displacement. PMID:25370027

Early Planetary Differentiation: Comparative Planetology

NASA Technical Reports Server (NTRS)

Jones, John H.

2006-01-01

We currently have extensive data for four different terrestrial bodies of the inner solar system: Earth, the Moon, Mars, and the Eucrite Parent Body [EPB]. All formed early cores; but all(?) have mantles with elevated concentrations of highly sidero-phile elements, suggestive of the addition of a late "veneer". Two appear to have undergone extensive differentiation consistent with a global magma ocean. One appears to be inconsistent with a simple model of "low-pressure" chondritic differentiation. Thus, there seems to be no single, simple paradigm for understand-ing early differentiation.

The Regolith of 4 Vesta - Inferences from Howardites

NASA Technical Reports Server (NTRS)

Mittlefehldt, D. W.; Herrin, J. S.; Cartwright, J. A.

2011-01-01

Asteroid 4 Vesta is quite likely the parent asteroid of the howardite, eucrite and diogenite meteorites - the HED clan. Eucrites and diogenites are the products of igneous processes; the former are basaltic composition rocks from flows, and shallow and deep intrusive bodies, whilst the latter are cumulate orthopyroxenites thought to have formed deep in the crust. Impact processes have excavated these materials and mixed them into a suite of polymict breccias. Howardites are polymict breccias composed mostly of clasts and mineral fragments of eucritic and diogenitic parentage, with neither end-member comprising more than 90% of the rock. Early work interpreted howardites as representing the lithified regolith of their parent asteroid. Recently, howardites have been divided into two subtypes; fragmental howardites, being a type of non-regolithic polymict breccia, and regolithic howardites, being lithified remnants of the active regolith of 4 Vesta. We are in the thralls of a collaborative investigation of the record of impact mixing contained within howardites, which includes studies of their mineralogy, petrology, bulk rock compositions, and bulk rock and clast noble gas contents. One goal of our investigation is to test the hypothesis that some howardites represent breccias formed from an ancient, well-mixed regolith on Vesta. Another is to use our results to further understand regolith processing on differentiated asteroids as compared to what has been learned from the Moon. We have made petrographic observations and electron microprobe analyses on 21 howardites and 3 polymict eucrites. We have done bulk rock analyses using X-ray fluorescence spectrometry and are completing inductively coupled plasma mass spectrometry analyses. Here, we discuss our petrologic and bulk compositional results in the context of regolith formation. Companion presentations describe the noble gas results and compositional studies of low-Ca pyroxene clasts.

THE PHYSICAL CHARACTERIZATION OF THE POTENTIALLY HAZARDOUS ASTEROID 2004 BL86: A FRAGMENT OF A DIFFERENTIATED ASTEROID

DOE Office of Scientific and Technical Information (OSTI.GOV)

Reddy, Vishnu; Sanchez, Juan A.; Takir, Driss

The physical characterization of potentially hazardous asteroids (PHAs) is important for impact hazard assessment and evaluating mitigation options. Close flybys of PHAs provide an opportunity to study their surface photometric and spectral properties that enable the identification of their source regions in the main asteroid belt. We observed PHA (357439) 2004 BL86 during a close flyby of the Earth at a distance of 1.2 million km (0.0080 AU) on 2015 January 26, with an array of ground-based telescopes to constrain its photometric and spectral properties. Lightcurve observations showed that the asteroid was a binary and subsequent radar observations confirmed themore » binary nature and gave a primary diameter of 300 m and a secondary diameter of 50–100 m. Our photometric observations were used to derive the phase curve of 2004 BL86 in the V-band. Two different photometric functions were fitted to this phase curve, the IAU H–G model and the Shevchenko model. From the fit of the H–G function we obtained an absolute magnitude of H = 19.51 ± 0.02 and a slope parameter of G = 0.34 ± 0.02. The Shevchenko function yielded an absolute magnitude of H = 19.03 ± 0.07 and a phase coefficient b = 0.0225 ± 0.0006. The phase coefficient was used to calculate the geometric albedo (Ag) using the relationship found by Belskaya and Schevchenko, obtaining a value of Ag = 40% ± 8% in the V-band. With the geometric albedo and the absolute magnitudes derived from the H–G and the Shevchenko functions we calculated the diameter (D) of 2004 BL86, obtaining D = 263 ± 26 and D = 328 ± 35 m, respectively. 2004 BL86 spectral band parameters and pyroxene chemistry are consistent with non-cumulate eucrite meteorites. A majority of these meteorites are derived from Vesta and are analogous with surface lava flows on a differentiated parent body. A non-diagnostic spectral curve match using the Modeling for Asteroids tool yielded a best-match with non-cumulate eucrite Bereba. Three other near-Earth asteroids (1993 VW, 1998 KK17, and 2000 XH44) that were observed by Burbine et al. also have spectral properties similar to 2004 BL86. The presence of eucrites with anomalous oxygen isotope ratios compared to the howardites, eucrites, and diogenites meteorites from Vesta suggests the possible presence of multiple differentiated bodies in the inner main belt or the contamination of Vesta’s surface with exogenic material. The spectral properties of both anomalous and Vestan eucrites are degenerate, making it difficult to identify the parent bodies of anomalous eucrites in the main belt and the NEO population using remote sensing. This makes it difficult to link 2004 BL86 directly to Vesta, although the Vesta family is the largest contributor of V-types to near-Earth space.« less

Carbonaceous Chondrite-Rich Howardites; The Potential for Hydrous Lithologies on the HED Parent

NASA Technical Reports Server (NTRS)

Herrin, J. S.; Zolensky, M. E.; Cartwright, J. A.; Mittlefehldt, D. W.; Ross, D. K.

2011-01-01

Howardites, eucrites, and diogenites, collectively referred to as the "HED's", are a clan of meteorites thought to represent three different lithologies from a common parent body. Collectively they are the most abundant type of achondrites in terrestrial collections. Eucrites are crustal basalts and gabbros, diogenites are mostly orthopyroxenites and are taken to represent lower crust or upper mantle materials, and howardites are mixed breccias containing both lithologies and are generally regarded as derived from the regolith or near-surface. The presence of exogenous chondritic material in howardite breccias has long been recognized. As a group, howardites exhibit divergence in bulk chemistry from what would be produced by mixing of diogenite and eucrite end-members exclusively, a phenomenon most evident in elevated concentrations of siderophile elements. Despite this chemical evidence for chondritic input in howardite breccias, chondritic clasts have only been identified in a minority of samples, and typically at levels of only a few percent. Three recent Antarctic howardite finds, the paired Mt. Pratt (PRA) 04401 and PRA 04402 and Scott Glacier (SCO) 06040, are notable for their high proportion of carbonaceous chondrite clasts. PRA 04401 is particularly well-endowed, with large chondritic clasts occupying more than half of the modal area of the sections we examined. Previously only a few percent chondritic clasts had been observed to occur in howardites. PRA 04401 is the most chondrite-rich howardite known

Mineralogy and Ar-39 - Ar-40 of an old pristine basalt: Thermal history of the HED parent body

NASA Technical Reports Server (NTRS)

Takeda, Hiroshi; Mori, Hiroshi; Bogard, Donald D.

1994-01-01

Previous investigations of mineral chemistry and Rb-Sr and Sm-Nd ages indicated that clast,84 from eucrite Yamato 75011 had preserved the pristine nature of its initial crystallization during an early stage of the HED parent body. Microscale mineralogy and Ar-39-Ar-40 ages of this clast, however, revealed local disturbance of microtextures and partially reset ages. This evidence suggests that, in addition to initial crystallization and rapid cooling, the Y75011,84 clast experienced shock deformation, reheating of short duration at higher temperature, and brecciation. These characteristics suggest two or more impact events. Fe-rich olivine filling fractures in pyroxene may have been introduced during the accompanying shock fracturing. The inferred Ar-39-Ar-40 degassing ages for Y75011 matrix and clast, 84 are 3.94 +/- 0.04 Ga and 3.98 +/- 0.03 Ga, respectively. The suggested degassing age for a clast from Y790020, believed to be paired with Y75011, is approximately 4.03 Ga, but could be younger. We consider it likely that all three samples experienced a common degassing event 3.95 +/- 0.05 Ga ago, but we cannot rule out two or more events spaced over a approximately 0.1 Ga interval. Higher temperature extractions of the two clast samples show significantly older apparent ages up to approximately 4.5 Ga and suggest that the time/temperature regime of this event was not sufficient to degas Ar totally. Most likely, the K-Ar ages were reset by thermal metamorphism associated with one or more impact events associated with shock fracturing, formation of Fe-rich olivine veins, and/or meteorite brecciation. The pyroxene annealing that commonly occurs in many eucrites is likely to be a much earlier process than the impact-produced textural changes and reset K-Ar ages observed in these meteorites. The existence of mineralogical and chronological evidence for metamorphism in an otherwise pristine eucrite suggests that the HED parent body experienced an extensive degree of early cratering.

Bulk Composition of Vesta as Constrained by the Dawn Mission and the HED Meteorites

NASA Technical Reports Server (NTRS)

Toplis, M. J.; Mizzon, H.; Forni, O.; Monnereau, H.; Prettyman, T. H.; McSween, H. Y.; McCoy, T. J.; Mittlefehldt, D. W.; DeSactis, M. C.; Raymond, C. T.;

Vestas Pinaria Region: Original Basaltic Achondrite Material Derived from Mixing Upper and Lower Crust

NASA Technical Reports Server (NTRS)

Mcfadden, L. A.; Combe, Jean-Philippe; Ammannito, Eleonora; Frigeri, Alessandro; Stephan, Katrin; Longobardo, Andrea; Palomba, Ernesto; Tosi, Federico; Zambon, Francesca; Krohn, Katrin;

ALHA 81011 -- an eucritic impact melt breccia formed 350 m.y. ago

NASA Astrophysics Data System (ADS)

Metzler, K.; Bobe, K. D.; Kunz, J.; Palme, H.; Spettel, B.; Stoeffler, D.

1994-07-01

The ALHA 81011 meteorite has been described as a eucritic breccia consisting of mineral and lithic clasts embedded in a vesicular, dark glassy matrix. Lithic clasts are equilibrated and dominated by subophitic and granulitic texture, frequently with gradual textural transitions in a given clast. Both mineral and lithic clasts were shocked in excess of approximately 30 GPa, transforming plagioclase into maskelynite, followed by thermally induced recrystallization. The observation that plagioclase fragments are 'swirled' into the dark matrix leaving pyroxene fragments unaffected, indicates that the plagioclase fragments were transformed into maskelynite prior to admixing as well. Scanning Electron Microscopy (SEM) investigations revealed that the dark matrix represents a quenched melt with eutectic fabric consisting of parallel intergrowths of pyroxene and plagioclase crystals, interspersed with small vesicles and larger subangular cavities up to 0.6 cm. One basalt clast with a partly granulitic texture and a portion of the dark crystallized matrix were separated and analyzed by Instrumental Neutron Activation Analysis (INAA). We performed age determinations on the separated lithologies by applying the Ar-40/AR-39 method. ALHA 81011 represents a clast-rich eucritic impact melt breccia not older than 350 Ma. It was either part of a rapidly cooled larger impact melt formation or represents a melt 'bomb' that originates from a suevitic ejecta blanket formed by a large-scale impact on the Howardite Eucritic and Diogenite (HED) parent body surface.

Petrography of isotopically-dated clasts in the Kapoeta howardite and petrologic constraints on the evolution of its parent body

NASA Technical Reports Server (NTRS)

Dymek, R. F.; Albee, A. L.; Chodos, A. A.; Wasserburg, G. J.

1976-01-01

Results are presented for petrographic and electron microprobe studies of the isotopically dated A, B, C, and rho basaltic rock fragments separated from the howardite Kapoeta. Other lithic clasts and numerous mineral fragments in thin sections of Kapoeta are investigated in order to outline the range in lithology and chemistry of the source materials from which the Kapoeta meteorite is derived. The data obtained are compared to those from other meteorite and lunar samples, with particular reference to the observational consequences for the evolution of the Kapoeta parent body. A major conclusion is that there is no clearcut evidence for young magmatism on the Kapoeta parent body. The observations preclude the interpretation that the Kapoeta is a simple mixture of eucrites and diogenites. In contrast to the moon, a source of anorthositic rocks does not appear to have been present on the Kapoeta parent body which involved chiefly pyroxene. The FeO-MnO relationships suggest that the source of the materials in the Kapoeta parent planet are fundamentally related.

Petrology of Anomalous Eucrites

NASA Technical Reports Server (NTRS)

Mittlefehldt, D. W.; Peng, Z. X.; Ross, D. K.

2015-01-01

Most mafic achondrites can be broadly categorized as being "eucritic", that is, they are composed of a ferroan low-Ca clinopyroxene, high-Ca plagioclase and a silica phase. They are petrologically distinct from angritic basalts, which are composed of high-Ca, Al-Ti-rich clinopyroxene, Carich olivine, nearly pure anorthite and kirschsteinite, or from what might be called brachinitic basalts, which are composed of ferroan orthopyroxene and high-Ca clinopyroxene, intermediate-Ca plagioclase and ferroan olivine. Because of their similar mineralogy and composition, eucrite-like mafic achondrites formed on compositionally similar asteroids under similar conditions of temperature, pressure and oxygen fugacity. Some of them have distinctive isotopic compositions and petrologic characteristics that demonstrate formation on asteroids different from the parent of the HED clan (e.g., Ibitira, Northwest Africa (NWA) 011). Others show smaller oxygen isotopic distinctions but are otherwise petrologically and compositionally indistinguishable from basaltic eucrites (e.g., Pasamonte, Pecora Escarpment (PCA) 91007). The degree of uniformity in delta O-17 of eucrites and diogenites is one piece of evidence considered to favor of a magma-ocean scenario for their petrogenesis. Given that the O isotopic differences separating Pasamonte and PCA 91007 from other eucrites are small, and that there is an absence of other distinguishing characteristics, a legitimate question is: Did the HED parent asteroid fail to homogenize via a magma-ocean stage, thus explaining outliers like Pasamonte? We are initiating a program of study of anomalous eucrite-like achondrites as one part of our effort to seek a resolution of this issue. Here we present preliminary petrologic information on Asuka (A-) 881394, Elephant Moraine (EET) 87520 and EET 87542. We will have studied several more by conference time.

Cosmogenic and fissiogenic noble gases and 81Kr-Kr exposure age clusters of eucrites

NASA Astrophysics Data System (ADS)

Shukolyukov, A.; Begemann, F.

1996-01-01

The isotopic composition and concentrations of noble gases were measured in the eucrites Bereba, Cachari, Caldera, Camel Donga, Chervony Kut, Ibitira, Jonzac, Juvinas, Millbillillie, Moore County, Padvarninkai, Pasamonte, Pomozdino, Serra de Magé, Sioux County, and Vetluga. The distribution of 81Kr-Kr exposure ages shows "clusters" at (7 ± 1) Ma, (10 ± 1) Ma, (14 ± 1) Ma, (22 ± 2) Ma, and (37 ± 1) Ma that agree with those for howardites, eucrites, and diogenites (HED) at (6 ± 1) Ma, (12 ± 2) Ma, (21 ± 4) Ma, and (38 ± 8) Ma. This most likely indicates a common origin of HED meteorites. Correlation equations for the shielding-sensitive cosmogenic ratios 78Kr/83Kr, 80Kr/83Kr, 82Kr/83Kr, and 124Xe/131Xe were obtained. Comparison with data from simulation experiments suggests that most eucrites were exposed to the cosmic radiation as somewhat large meteoroids with diameters of ˜1 m or more. The shielding-dependence of the 78Kr and 126Xe production rates was found to be small, with a few exceptions the variations aren <10%-15%. Concentrations of spallogenic 3He indicate diffusive losses of up to 70% that can be, in first approximation, described by a model of quasi-continuous losses during the exposure to the cosmic radiation with a loss rate of the order of ˜3 × 10-8 a-1. Radiogenic 4He shows additional substantial losses that occurred at the time of, or prior to, the separation of the meteoroids from their parent body. Typical 40Ar retention in eucrites is 50%-60% which corresponds to a 40Ar-K retention age of 3.4-3.6 Ga. In all analyzed unbrecciated eucrites, the retention is distinctly larger (70%-100%). The 244Pu fission ratio (86Kr/136Xe)Pu, was evaluated from the data on Pomozdino samples to be 0.039 ± 0.014.

Experimental Constraints on a Vesta Magma Ocean

NASA Technical Reports Server (NTRS)

Hoff, C.; Jones, J. H.; Le, L.

2014-01-01

A magma ocean model was devised to relate eucrites (basalts) and diogenites (orthopyroxenites), which are found mixed together as clasts in a suite of polymict breccias known as howardites. The intimate association of eucritic and diogenitic clasts in howardites argues strongly that these three classes of achondritic meteorites all originated from the same planetoid. Reflectance spectral evidence (including that from the DAWN mission) has long suggested that Vesta is indeed the Eucrite Parent Body. Specifically, the magma ocean model was generated as follows: (i) the bulk Vesta composition was taken to be 0.3 CV chondrite + 0.7 L chondrite but using only 10% of the Na2O from this mixture; (ii) this composition is allowed to crystallize at 500 bar until approx. 80% of the system is solid olivine + low-Ca pyroxene; (iii) the remaining 20% liquid crystallizes at one bar from 1250C to 1110C, a temperature slightly above the eucrite solidus. All crystallization calculations were performed using MELTS. In this model, diogenites are produced by cocrystallization of olivine and pyroxene in the >1250C temperature regime, with Main Group eucrite liquids being generated in the 1300-1250C temperature interval. Low-Ca pyroxene reappears at 1210C in the one-bar calculations and fractionates the residual liquid to produce evolved eucrite compositions (Stannern Trend). We have attempted to experimentally reproduce the <1250C portion of the MELTS Vesta magma ocean. In the MELTS calculation, the change from 500 bar to one bar results in a shift of the olivine:low-Ca pyroxene boundary so that the 1250C liquid is now in the olivine field and, consequently, olivine should be the first-crystallizing phase, followed by low-Ca pyroxene at 1210C, and plagioclase at 1170C. Because at one bar the olivine:low-Ca pyroxene boundary is a peritectic, fractional crystallization of the 1210C liquid proceeds with only pyroxene crystallization until plagioclase appears. Thus, the predictions of the MELTS calculation are clear and straightforward.

Geochemical evidence for the formation of the Moon by impact induced fission of the proto-Earth

NASA Technical Reports Server (NTRS)

Waenke, H.; Dreibus, G.

1984-01-01

Geochemical evidence is discussed which advocates the theory that the Moon was formed by impact induced fission of the Earth. The Earth's mantle exhibits a number of geochemical peculiarities which make our planet a unique object in the solar system. Terrestrial basalts are compared with those from the Eucrite parent body and the Shergotty parent body. Also the Moon's composition is very close to the Earth's in all details except the lower FeO content which is explained. Evidence is discussed for the plausible physical process of formation of the Moon by impact induced fission. Also the theory that impact induced fission occurred at the moment at which accretion of the Earth was not totally complete is briefly discussed.

Cosmic-Ray-Exposure Ages of Diogenites and the Collisional History of the HED Parent Body or Bodies

NASA Technical Reports Server (NTRS)

Welten, K. C.; Lindner, L.; vanderBorg, K.; Loeken, T.; Scherer, P.; Schultz, L.

1996-01-01

Cosmic-ray-exposure ages of meteorites provide information on the collisional history of their parent bodies and the delivery mechanism of meteorites to Earth. The exposure-age distributions of ordinary chondrites show distinct patterns for H, L, and LL types, consistent with their origin on different parent bodies. The exposure-age distributions of howardites, eucrites. and diogenites (HEDS) show a common pattern with major peaks at 22 Ma and 38 Ma This provides additional evidence for a common origin of the HED meteorites, possibly 4 Vesta, although orbital dynamics calculations showed that the delivery of meteorites from Vesta to Earth is difficult. However, the discovery of several kilometer-sized Vesta-like asteroids in the region between Vesta and the 3:1 resonance suggested that these seem more likely parent bodies of the HEDs than Vesta itself. This implies that the exposure-age clusters may represent samples of several parent bodies. Therefore, the near-absence of diogenites with ages <20 Ma might be of interest for the composition of these kilometer-sized fragments of Vesta. Here we present cosmic-ray-exposure ages of 20 diogenites, including 9 new meteorites. In addition, we calculate the probability for each peak to occur by chance, assuming a constant production rate of HED fragments.

Petrology and Geochemistry of Unbrecciated Harzburgitic Diogenite MIL 07001: A Window Into Vestan Geological Evolution

NASA Technical Reports Server (NTRS)

Mittlefehldt, D. W.; Peng, Z. X.; Mertzman, S. A.; Mertzman, K. R.

2014-01-01

There is a strong case that asteroid 4 Vesta is the parent of the howardite, eucrite and diogenite (HED) meteorites. Models developed for the geological evolution of Vesta can satisfy the compositions of basaltic eucrites that dominate in the upper crust. The bulk compositional characteristics of diogenites - cumulate harzburgites and orthopyroxenites from the lower crust - do not fit into global magma ocean models that can describe the compositions of basaltic and cumulate eucrites. Recent more detailed formation models do make provision for a more complicated origin for diogenites, but this model has yet to be completely vetted. Compositional studies of bulk samples has led to the hypothesis that many diogenites were formed late by interaction of their parent melts with a eucritic crust, but those observations may alternatively be explained by subsolidus equilibration of trace elements between orthopyroxene and plagioclase and Ca-phosphate in the rocks. Differences in radiogenic Mg-26 content between diogenites and eucrites favors early formation of the former, not later formation. Understanding the origin of diogenites is crucial for understanding the petrologic evolution of Vesta. We have been doing coordinated studies of a suite of diogenites including petrologic investigations, bulk rock major and trace element studies, and in situ trace element analyses of orthopyroxene. Here we will focus on an especially unusual, and potentially key, diogenite, MIL 07001.

Characterization of crust formation on a parent body of achondrites and the moon by pyroxene crystallography and chemistry

NASA Technical Reports Server (NTRS)

Takeda, H.; Miyamoto, M.; Ishii, T.; Reid, A. M.

1976-01-01

Single crystal X-ray diffraction and electron microprobe techniques were used to study lunar crustal pyroxenes in a cataclastic norite, a pyroxene-rich clast, and anorthosite lunar samples, and also in meteorites including diogenites, eucrites, and the Yamoto (1) howardite. The crystallographic and chemical characteristics of pyroxenes in these materials are compared and are discussed in terms of the lower stability limit of pigeonite. A mechanical mixing model of howardite is proposed.

Catching Constrains on the Parent Body Genesis of Mesosiderites and a Possible Link to HED (Howardite-Eucrite-Diogenite) Meteorites - A New Hope?

NASA Technical Reports Server (NTRS)

Baecker, B.; Cohen, Barbara A.

2016-01-01

Mesosiderites (MES) are a group of enigmatic stony-iron meteorites exhibiting fragmental matrix breccias and irregular textures; e.g. [1-3]. Mesosiderites contain roughly equal volumes metal (Fe-Ni) and silicates often intimately mixed together (Fig.1). The silicates mostly consist of basaltic, gabbroic, and pyroxenitic components, and appear similar to eucrites and howardites; [4-8]. But unlike HEDs - and other differentiated parent body meteorite groups e.g. ureilites - mesosiderites contain high metal abundances. Several studies have been published to reveal the processes leading to the formation of mesosiderites and attempt to classifiy them [1], [2], [10-15]. Because the silicate inclusions in mesosiderites are often strongly metamorphosed after formation, it is difficult to assess the origin of the silicates and implications for the differentiation process of their parent body [15-17]. Several workers have advanced a formation hypothesis for the mesosiderites where an impact between differentiated bodies occurred prior to 4.47 Ga ago (e.g. [13,18], which could explain the possible incomplete dispersal of the colliding bodies due to their low cosmic ray exposure ages and their special thermal history. However, [13] discuss and favor the model for formation of mesosiderites with the collision of two differentiated bodies, along with disruption events and gravitational re-assembly. The mesosiderites have numerous gabbroid melt clasts with anomalous rare-earth- element (REE) - especially positive Eu - values [19, 20]. HEDs do not show the same. However, the heating mechanisms of both mesosiderites and HED's are puzzling. Mesosiderites are remarkable, they consist of a mix of basalts, which are only found on or near planetary surfaces and undifferentiated metal [1,2]. The probable model is that an asteroid containing a metallic magma impacted onto a second asteroid covered with basalt [18,21]. The mix was then buried under an insulating regolith, and cooled slowly. During cooling and at low temperatures the redox reactions continued to occur and proceed (J.T. Wasson; in pers. comm. 2015).

Petrology and geochemistry of the unbrecciated achondrite Northwest Africa 1240 (NWA 1240): an HED parent body impact melt

NASA Astrophysics Data System (ADS)

Barrat, J. A.; Jambon, A.; Bohn, M.; Blichert-Toft, J.; Sautter, V.; Göpel, C.; Gillet, Ph.; Boudouma, O.; Keller, F.

2003-10-01

NWA 1240 is an unusual eucrite recently recovered in Morocco as a single stone of 98 g. It is an unbrecciated greenish-brown rock nearly devoid of fusion crust. It displays porphyritic texture consisting of skeletal hollow low-Ca pyroxene phenocrysts set in a variolitic (fan-spherulitic) mesostasis of fine elongate pyroxene and plagioclase crystals. Minor phases are skeletal chromite, iron, silica, troilite, ilmenite and minute amounts of phosphate and fayalite. Pyroxenes are unequilibrated and show one of the widest ranges of composition so far described for a eucrite, from En 76.0Wo 1.9Fs 22.1 to compositions nearly devoid of Mg (unusual ferrosilite and Fe-augite symplectites and possibly pyroxferroite). Plagioclase crystals contain significant amounts of Fe and Mg, which are possibly controlled by the Ca(Mg,Fe 2+)Si 3O 8 plagioclase component. To discuss the potential effects of hot-desert weathering on NWA 1240, we have analyzed a series of Saharan eucrites (Agoult, Aoufous, Igdi, Smara, NWA 047 and NWA 049) and large aliquots (0.39 to 2.8 g) of eucrite falls (Bereba, Bouvante, Jonzac, Juvinas and Serra de Magé). These results indicate that among the elements we have determined, Pb, Ba and Sr are the most sensitive indicators of Saharan weathering. The bulk composition of NWA 1240 has been determined for 45 elements by ICP-AES and ICP-MS. The data show that the meteorite is not significantly weathered: its Pb concentration is very low; Ba and Sr concentrations are not anomalously high; the Th/U and Hf/Sm ratios are chondritic (Th/U = 3.65, Hf/Sm = 0.74). NWA 1240 is rich in MgO (10.4 wt%) and Cr 2O 3 (0.71 wt%), and displays striking similarities with cumulate eucrites, such as having similar incompatible trace element patterns and a significant positive Eu anomaly (Eu/Eu* = 1.37). The combination of fast cooling and cumulate eucrite-dominated composition suggests that NWA 1240 is not an igneous rock but rather an impact melt.

Do Mesosiderites Reside on 4 VESTA? an Assessment Based on Dawn Grand Data

NASA Technical Reports Server (NTRS)

Mittlefehldt, D. W.; Prettyman, T. H.; Reedy, R. C.; Beck, A. W.; Blewett, D. T.; Gaffey, M. J.; Lawrence, D. J.; McCoy, T. J.; McSween, H. Y., Jr.; Toplis, J. J.

2012-01-01

Almost a century ago, simple petrographic observations were used to suggest a close genetic link between eucrites and the silicates in mesosiderites [1]. Mesosiderites are composed of roughly equal proportions of silicates that are very similar in mineralogy and texture to howardites, and Fe, Ni metal (Fig. 1) [2]. This similarity has led some to conclude that mesosiderites come from the howardite, eucrite and diogenite (HED) parent asteroid [3, 4]. Subsequent petrologic study demonstrated a number of differences between mesosiderite silicates and HEDs that are more plausibly explained as requiring separate parent asteroids [5]. However, HEDs and mesosiderites are identical in oxygen isotopic composition, and this has been used to argue for a common parent 4 Vesta [6].

Meteorite Dunite Breccia MIL 03443: A Probable Crustal Cumulate Closely Related to Diogenites from the HED Parent Asteroid

NASA Technical Reports Server (NTRS)

Mittlefehldt, David W.

2008-01-01

There are numerous types of differentiated meteorites, but most represent either the crusts or cores of their parent asteroids. Ureilites, olivine-pyroxene-graphite rocks, are exceptions; they are mantle restites [1]. Dunite is expected to be a common mantle lithology in differentiated asteroids. In particular, models of the eucrite parent asteroid contain large volumes of dunite mantle [2-4]. Yet dunites are very rare among meteorites, and none are known associated with the howardite, eucrite, diogenite (HED) suite. Spectroscopic measurements of 4 Vesta, the probable HED parent asteroid, show one region with an olivine signature [5] although the surface is dominated by basaltic and orthopyroxenitic material equated with eucrites and diogenites [6]. One might expect that a small number of dunitic or olivine-rich meteorites might be delivered along with the HED suite. The 46 gram meteoritic dunite MIL 03443 (Fig. 1) was recovered from the Miller Range ice field of Antarctica. This meteorite was tentatively classified as a mesosiderite because large, dunitic clasts are found in this type of meteorite, but it was noted that MIL 03443 could represent a dunite sample of the HED suite [7]. Here I will present a preliminary petrologic study of two thin sections of this meteorite.

A numerical model of the physical and chemical evolution of Vesta

NASA Astrophysics Data System (ADS)

Mizzon, H.; Monnereau, M.; Toplis, M. J.; Prettyman, T. H.; McSween, H. Y.; Raymond, C. A.; Russell, C. T.

2015-10-01

Vesta is a 262 km radius asteroid that has been proposed as the parent body of the Howardite- Eucrite-Diogenite family of meteorites. The observations of the Dawn spacecraft confirm the idea that this protoplanet underwent magmatic differentiation, providing evidence for regions of the upper crust rich in basaltic (eucritic) lithologies, while regions that have experienced excavation related to large impacts (i.e. Rheasilvia) are richer in pyroxene-dominated (diogenitic) lithologies [1,2]. One of the most striking results of the Dawn mission is the absence of olivine at the near-surface, even in the deep Rheasiliva basin. This observation has been used to question the chondritic nature of bulk Vesta and/or question its status as an intact protoplanet [3]. From a geochemical point of view, the HED meteorites are consistent with chondritic precursors [4], but petrological models have met difficulties explaining both eucrites and diogenites in a unified way [5]. These models comprise two extreme endmember scenarios: the first considers the partial melting of the primitive mantle of Vesta, followed by melt extraction [6], while the second involves the solidification of an initially entirely molten magma ocean [7]. In the latter case, major-element chemistry of eucrites and diogenites can be reproduced [7], but not the extreme range of trace element concentrations observed in diogenites [8]. More importantly, the physics of melt migration seems to preclude the existence of a global magma ocean, assuming that 26Al is the only heat source capable of extensively producing melt in early small bodies. This is because plagioclase is one of the first phases to melt, thus early formed liquids are Al-rich. Rapid migration of such liquids redistributes 26Al, limiting melt production where liquid has been lost [9,10]. This idea was explored by [11], who qualitatively suggested that the first melts formed would migrate to the surface (as eucrites), while the lower mantle would become enriched in refractory olivine through its downward compaction. This last point potentially explains the lack of this mineral near Vesta's surface. The aim of work presented here is to quantitatively explore this idea by computing the mineralogy as a function of depth and time, using a set of numerical solutions of conservative equations and an appropriate phase diagram.

Early solar system. Early accretion of water in the inner solar system from a carbonaceous chondrite-like source.

PubMed

Sarafian, Adam R; Nielsen, Sune G; Marschall, Horst R; McCubbin, Francis M; Monteleone, Brian D

2014-10-31

Determining the origin of water and the timing of its accretion within the inner solar system is important for understanding the dynamics of planet formation. The timing of water accretion to the inner solar system also has implications for how and when life emerged on Earth. We report in situ measurements of the hydrogen isotopic composition of the mineral apatite in eucrite meteorites, whose parent body is the main-belt asteroid 4 Vesta. These measurements sample one of the oldest hydrogen reservoirs in the solar system and show that Vesta contains the same hydrogen isotopic composition as that of carbonaceous chondrites. Taking into account the old ages of eucrite meteorites and their similarity to Earth's isotopic ratios of hydrogen, carbon, and nitrogen, we demonstrate that these volatiles could have been added early to Earth, rather than gained during a late accretion event. Copyright © 2014, American Association for the Advancement of Science.

Chondritic models of 4 Vesta: Implications for geochemical and geophysical properties

NASA Astrophysics Data System (ADS)

Toplis, M. J.; Mizzon, H.; Monnereau, M.; Forni, O.; McSween, H. Y.; Mittlefehldt, D. W.; McCoy, T. J.; Prettyman, T. H.; De Sanctis, M. C.; Raymond, C. A.; Russell, C. T.

2013-11-01

Simple mass-balance and thermodynamic constraints are used to illustrate the potential geochemical and geophysical diversity of a fully differentiated Vesta-sized parent body with a eucrite crust (e.g., core size and density, crustal thickness). The results of this analysis are then combined with data from the howardite-eucrite-diogenite (HED) meteorites and the Dawn mission to constrain Vesta's bulk composition. Twelve chondritic compositions are considered, comprising seven carbonaceous, three ordinary, and two enstatite chondrite groups. Our analysis excludes CI and LL compositions as plausible Vesta analogs, as these are predicted to have a negative metal fraction. Second, the MELTS thermodynamic calculator is used to show that the enstatite chondrites, the CV, CK and L-groups cannot produce Juvinas-like liquids, and that even for the other groups, depletion in sodium is necessary to produce liquids of appropriate silica content. This conclusion is consistent with the documented volatile-poor nature of eucrites. Furthermore, carbonaceous chondrites are predicted to have a mantle too rich in olivine to produce typical howardites and to have Fe/Mn ratios generally well in excess of those of the HEDs. On the other hand, an Na-depleted H-chondrite bulk composition is capable of producing Juvinas-like liquids, has a mantle rich enough in pyroxene to produce abundant howardite/diogenite, and has a Fe/Mn ratio compatible with eucrites. In addition, its predicted bulk-silicate density is within 100 kg m-3 of solutions constrained by data of the Dawn mission. However, oxidation state and oxygen isotopes are not perfectly reproduced and it is deduced that bulk Vesta may contain approximately 25% of a CM-like component. Values for the bulk-silicate composition of Vesta and a preliminary phase diagram are proposed.

Chemical Mixing Model and K-Th-Ti Systematics and HED Meteorites for the Dawn Mission

NASA Technical Reports Server (NTRS)

Usui, T.; McSween, H. Y., Jr.; Mittlefehldt, D. W.; Prettyman, T. H.

2009-01-01

The Dawn mission will explore 4 Vesta, a large differentiated asteroid believed to be the parent body of the howardite, eucrite and diogenite (HED) meteorite suite. The Dawn spacecraft carries a gamma-ray and neutron detector (GRaND), which will measure the abundances of selected elements on the surface of Vesta. This study provides ways to leverage the large geochemical database on HED meteorites as a tool for interpreting chemical analyses by GRaND of mapped units on the surface of Vesta.

Bunburra Rockhole: Exploring the geology of a new differentiated asteroid

NASA Astrophysics Data System (ADS)

Benedix, G. K.; Bland, P. A.; Friedrich, J. M.; Mittlefehldt, D. W.; Sanborn, M. E.; Yin, Q.-Z.; Greenwood, R. C.; Franchi, I. A.; Bevan, A. W. R.; Towner, M. C.; Perrotta, G. C.; Mertzman, S. A.

2017-07-01

Bunburra Rockhole is the first recovered meteorite of the Desert Fireball Network. We expanded a bulk chemical study of the Bunburra Rockhole meteorite to include major, minor and trace element analyses, as well as oxygen and chromium isotopes, in several different pieces of the meteorite. This was to determine the extent of chemical heterogeneity and constrain the origin of the meteorite. Minor and trace element analyses in all pieces are exactly on the basaltic eucrite trend. Major element analyses show a slight deviation from basaltic eucrite compositions, but not in any systematic pattern. New oxygen isotope analyses on 23 pieces of Bunburra Rockhole shows large variation in both δ17O and δ18O, and both are well outside the HED parent body fractionation line. We present the first Cr isotope results of this rock, which are also distinct from HEDs. Detailed computed tomographic scanning and back-scattered electron mapping do not indicate the presence of any other meteoritic contaminant (contamination is also unlikely based on trace element chemistry). We therefore conclude that Bunburra Rockhole represents a sample of a new differentiated asteroid, one that may have more variable oxygen isotopic compositions than 4 Vesta. The fact that Bunburra Rockhole chemistry falls on the eucrite trend perhaps suggests that multiple objects with basaltic crusts accreted in a similar region of the Solar System.

Dawn and the Vesta-HED Connection

NASA Technical Reports Server (NTRS)

McSween, H. Y.; Mittlefehldt, D. W.; Beck, A. W.; McCoy, T.; Marchi, S.; DeSanctis, M. C.; Ammannito, E.; Raymond, C. A.; Russell, C. T.

2012-01-01

Although it is difficult to explain exactly how eucrites and diogenites are related through simple magmatic processes, their shared oxygen isotopic compositions and the common occurrence of clasts of both lithologies in howardite breccias support derivation from a common parent body. For decades, HED meteorites have been linked to asteroid 4 Vesta, based on spectral similarities [1] and the discovery of a dynamical family (Vestoids) that provides a bridge between Vesta and nearby resonance escape hatches [2]. Although recently derived constraints on the rapidity of HED parent body differentiation, based on measurements of Al-26 in diogenites, have been used to argue against the Vesta-HED connection [3], new thermal evolution models [e.g., 4] appear to be heated and melted fast enough to account for this constraint. Data from the Dawn orbiter strengthen the Vesta - HED linkage and provide new insights into petrogenetic interpretations of these meteorites.

Compositions of Normal and Anomalous Eucrite-Type Mafic Achondrites

NASA Technical Reports Server (NTRS)

Mittlefehldt, D. W.; Peng, Z. X.; Mertzman, S. A.

2016-01-01

The most common asteroidal igneous meteorites are eucrite-type mafic achondrites - basalts and gabbros composed of ferroan pigeonite, ferroan augite, calcic plagioclase, silica, ilmenite, troilite, Ca-phosphate, chromite and Fe-metal. These rocks are thought to have formed on a single asteroid along with howardites and diogenites. However, high precision O-isotopic analyses have shown that some mafic achondrites have small, well-resolved, non-mass-dependent differences that have been interpreted as indicating derivation from different asteroids. Some of these O-anomalous mafic achondrites also have anomalous petrologic characteristics, strengthening the case that they hail from distinct parent asteroids. We present the results of bulk compositional studies of a suite of normal and anomalous eucrite-type basalts and cumulate gabbros.

REE Partition Coefficients from Synthetic Diogenite-Like Enstatite and the Implications of Petrogenetic Modeling

NASA Technical Reports Server (NTRS)

Schwandt, C. S.; McKay, G. A.

1996-01-01

Determining the petrogenesis of eucrites (basaltic achondrites) and diogenites (orthopyroxenites) and the possible links between the meteorite types was initiated 30 years ago by Mason. Since then, most investigators have worked on this question. A few contrasting theories have emerged, with the important distinction being whether or not there is a direct genetic link between eucrites and diogenites. One theory suggests that diogenites are cumulates resulting from the fractional crystallization of a parent magma with the eucrites crystallizing, from the residual magma after separation from the diogenite cumulates. Another model proposes that diogenites are cumulates formed from partial melts derived from a source region depleted by the prior generation of eucrite melts. It has also been proposed that the diogenites may not be directly linked to the eucrites and that they are cumulates derived from melts that are more orthopyroxene normative than the eucrites. This last theory has recently received more analytical and experimental support. One of the difficulties with petrogenetic modeling is that it requires appropriate partition coefficients for modeling because they are dependent on temperature, pressure, and composition. For this reason, we set out to determine minor- and trace-element partition coefficients for diogenite-like orthopyroxene. We have accomplished this task and now have enstatite/melt partition coefficients for Al, Cr, Ti, La, Ce, Nd, Sm, Eu, Dy, Er, Yb, and La.

Volatile Concentrations and H-Isotope Composition of Unequilibrated Eucrites

NASA Technical Reports Server (NTRS)

Sarafian, Adam R.; Nielsen, Sune G.; Marschall, Horst R.; Gaetani, Glenn A.; Hauri, Erik H.; Righter, Kevin; Berger, Eve L.

2017-01-01

Eucrites are among the oldest and best studied asteroidal basalts (1). They represent magmatism that occurred on their parent asteroid, likely 4-Vesta, starting at 4563 Ma and continuing for approx. 30 Myr. Two hypotheses are debated for the genesis of eucrites, a magma ocean model (2), and a mantle partial melting model. In general, volatiles (H, C, F, Cl) have been ignored for eucrites and 4-Vesta, but solubility of wt% levels of H2O are possible at Vestan interior PT conditions. Targeted measurements on samples could aid our understanding considerably. Recent studies have found evidence of volatile elements in eucrites, but quantifying the abundance of volatiles remains problematic (6). Volatile elements have a disproportionately large effect on melt properties and phase stability, relative to their low abundance. The source of volatile elements can be elucidated by examining the hydrogen isotope ratio (D/H), as different H reservoirs have drastically different H isotope compositions. Recent studies of apatite in eucrites have shown that the D/H of 4-Vesta matches that of Earth and carbonaceous chondrites, however, the D/H of apatites may not represent the D/H of a primitive 4-Vesta melt due to the possibility of degassing prior to the crystallization of apatite. Therefore, the D/H of early crystallizing phases must be measured to determine if the D/H of 4-Vesta is equal to that of the Earth and carbonaceous chondrites.

Chemistry of Diogenites and Evolution of their Parent Asteroid

NASA Technical Reports Server (NTRS)

Mittlefehldt, D.W.; Beck, A.W.; McSween, H.Y.; Lee, C-T A.

2009-01-01

Diogenites are orthopyroxenite meteorites [1]. Most are breccias, but remnant textures indicate they were originally coarse-grained rocks, with grain sizes of order of cm. Their petrography, and major and trace element chemistry support an origin as crustal cumulates from a differentiated asteroid. Diogenites are genetically related to the basaltic and cumulate-gabbro eucrites, and the polymict breccias known as howardites, collectively, the HED suite. Spectroscopic observations, orbit data and dynamical arguments strongly support the hypothesis that asteroid 4 Vesta is the parent object for HED meteorites [2]. Here we discuss our new trace element data for a suite of diogenites and integrate these into the body of literature data. We use the combined data set to discuss the petrologic evolution of diogenites and 4 Vesta.

Photomosaics of the cathodoluminescence of 60 sections of meteorites and lunar samples

USGS Publications Warehouse

Akridge, D.G.; Akridge, J.M.C.; Batchelor, J.D.; Benoit, P.H.; Brewer, J.; DeHart, J.M.; Keck, B.D.; Jie, L.; Meier, A.; Penrose, M.; Schneider, D.M.; Sears, D.W.G.; Symes, S.J.K.; Yanhong, Z.

2004-01-01

Cathodoluminescence (CL) petrography provides a means of observing petrographic and compositional properties of geological samples not readily observable by other techniques. We report the low-magnification CL images of 60 sections of extraterrestrial materials. The images we report include ordinary chondrites (including type 3 ordinary chondrites and gas-rich regolith breccias), enstatite chondrites, CO chondrites and a CM chondrite, eucrites and a howardite, lunar highland regolith breccias, and lunar soils. The CL images show how primitive materials respond to parent body metamorphism, how the metamorphic history of EL chondrites differs from that of EH chondrites, how dark matrix and light clasts of regolith breccias relate to each other, how metamorphism affects eucrites, the texture of lunar regolith breccias and the distribution of crystallized lunar spherules ("lunar chondrules"), and how regolith working affects the mineral properties of lunar soils. More particularly, we argue that such images are a rich source of new information on the nature and history of these materials and that our efforts to date are a small fraction of what can be done. Copyright 2004 by the American Geophysical Union.

Northwest Africa 1401: A Polymict Cumulate Eucrite with a Unique Ferroan Heteradcumulate Mafic Clast

NASA Technical Reports Server (NTRS)

Mittlefehldt, David W.; Killgore, Marvin

2003-01-01

The howardite, eucrite and diogenite (HED) clan is the largest suite of achondrites available for study. The suite gives us a unique view of the magmatism that affected some asteroids early in solar system history. One problem with mining the HED clan for petrogenetic information is that there is only limited petrologic diversity among the rock types. Thus, discovering unusual HED materials holds the potential for revealing new insights into the petrologic evolution of the HED parent asteroid. Here we report on petrologic study of an unusual, 27 gram polymict eucrite, Northwest Africa (NWA) 1401. The thin section studied (approx. 20 x 10 mm) contains one large, ferroan clast described separately. The remainder of the rock, including mineral fragments and other, smaller lithic clasts, forms the host breccia.

The behaviour of tungsten during mantle melting revisited with implications for planetary differentiation time scales

NASA Astrophysics Data System (ADS)

Babechuk, Michael G.; Kamber, Balz S.; Greig, Alan; Canil, Dante; Kodolányi, János

2010-02-01

Tungsten is a moderately siderophile high-field-strength element that is hydrophile and widely regarded as highly incompatible during mantle melting. In an effort to extend empirical knowledge regarding the behaviour of W during the latter process, we report new high-precision trace element data (W, Th, U, Ba, La, Sm) that represent both terrestrial and planetary reservoirs: MORB (11), abyssal peridotites (8), eucrite basalts (3), and carbonaceous chondrites (8). A full trace element suite is also reported for Cordilleran Permian ophiolite peridotites (12) to better constrain the behaviour of W in the upper mantle. In addition, we report our long-term averages for a number of USGS (BIR-1, BHVO-1, BHVO-2, PCC-1, DTS-1) and GSJ (JA-3, JP-1) standard reference materials, some of which we conclude to be heterogeneous and contaminated with respect to W. The most significant finding of this study is that many of the highly depleted upper mantle peridotites contain far higher W concentrations than expected. In the absence of convincing indications for alteration, re-enrichment or contamination, we propose that the W excess was caused by retention in an Os-Ir alloy phase, whose stability is dependent on fO 2 of the mantle source region. This explanation could help to account for the particularly low W content of N-MORB and implies that the lithophile behaviour of W in basaltic rocks is not an accurate representation of the behaviour in the melt source. These findings then become relevant to the interpretation of W-isotopic data for achondrites, where the fractionation of Hf from W during melting is used to infer the Hf/W of the parent body mantle. This is exemplified by the differentiation chronology of the eucrite parent body (EPB), which has been modeled with a melt source with high Hf/W. By contrast, we explore the alternative scenario with a low mantle Hf/W on the EPB. Using available eucrite literature data, a maximum core segregation age of 1.2 ± 1.2 Myr after the closure of CAIs is calculated with a more prolonged time between core formation and mantle fractionation of ca. 2 Myr. This timeline is consistent with most recent published chronologies of the EPB differentiation based on the 53Mn- 53Cr and 26Al- 26Mg systems.

FE-60 and the evolution of eucrites

NASA Technical Reports Server (NTRS)

Shukolyukov, A.; Lugmair, G. W.

1993-01-01

We have recently presented evidence for the existence of live Fe-60 in the early solar system. This evidence comes from observations of 2.4 to 50 epsilon unit (1 part in 10(exp 4)) relative excesses of Ni-60 measured in samples from the eucrite Chervony Kut (CK). These isotopic excesses have been produced by the decay of the short-lived radionuclide Fe-60 (T(sub 1/2) = 1.5 Ma). Because CK originates from a planetesimal which was totally molten and its high Fe/Ni ratio is due to a planet-wide Fe-Ni fractionation during metal-silicate segregation, the presence of the Fe-60 decay product indicates the large scale abundance of Fe-60 in the early solar system and its presence during differentiation of this planetesimal. The observed variable Ni-60 excesses in different bulk samples and mineral separates from CK can only be understood if some Fe-60 was still alive at the time when basaltic magma had solidified on the eucrite parent body. The lack of a correlation between Ni-60 and the respective Fe/Ni ratios in different mineral fractions from CK indicates a metamorphic remobilization of Ni after essentially all Fe-60 has decayed. However, Ni-60 from three bulk samples from different locations within the meteorite appears to correlate reasonably well with the respective Fe/Ni ratios. If we regard this correlation as an isochron then its slope yields a Fe-60/Fe-56 ratio f (3.9 +/- 0.6) x 10(exp -9) and an initial Ni-60 of 3.2 plus or minus 0.9 epsilon units at the time of crystallization of CK. Estimates based on these values and a approximately 10 Ma time interval between CK solidification and formation of the earliest condensates in the solar system followed by rapid accretion of planetary bodies indicate that the decay of Fe-60 could produce sufficient heat to melt these planetesimals. If Al-26 was present on a planetary scale as Fe-60 and at abundances close to values observed in Allende inclusions then melting of small early formed planets is inevitable. As an attempt to further explore the Fe-60/Ni-60 isotope system as an early solar system chronometer we studied another noncumulate eucrite, Juvinas (JUV) (sample USNM 1051), which belongs to the same subgroup as CK.

Asteroid-Meteorite Links: The Vesta Conundrum(s)

NASA Technical Reports Server (NTRS)

Pieters, C. M.; Binzel, R.; Bogard, D.; Hiroi, T.; Mittlefehldt, D. W.; Nyquist, L.; Rivkin, A.; Takeda, H.

2006-01-01

Although a direct link between the HED meteorites and the asteroid 4 Vesta is generally acknowledged, several issues continue to be actively examined that tie Vesta to early processes in the solar system. Vesta is no longer the only basaltic asteroid in the Main belt. In addition to the Vestoids of the Vesta family, the small asteroid Magnya is basaltic but appears to be unrelated to Vesta. Similarly, diversity now identified in the collection of basaltic meteorites requires more than one basaltic parent body, consistent with the abundance of differentiated parent bodies implied by iron meteorites. The timing of the formation of the Vestoids (and presumably the large crater at the south pole of Vesta) is unresolved. Peaks in Ar-Ar dates of eucrites suggest this impact event could be related to a possible late heavy bombardment at least 3.5 Gyr ago. On the other hand, the optically fresh appearance of both Vesta and the Vestoids requires either a relatively recent resurfacing event or that their surfaces do not weather in the same manner thought to occur on other asteroids such as the ordinary chondrite parent body. Diversity across the surface of Vesta has been observed with HST and there are hints of compositional variations (possibly involving minor olivine) in near-infrared spectra.

Differentiation and magmatic activity in Vesta evidenced by 26Al-26Mg dating in eucrites and diogenites

NASA Astrophysics Data System (ADS)

Hublet, G.; Debaille, V.; Wimpenny, J.; Yin, Q.-Z.

2017-12-01

The 26Al-26Mg short-lived chronometer has been widely used for dating ancient objects in studying the early Solar System. Here, we use this chronometer to investigate and refine the geological history of the asteroid 4-Vesta. Ten meteorites widely believed to come from Vesta (4 basaltic eucrites, 3 cumulate eucrites and 3 diogenites) and the unique achondrite Asuka 881394 were selected for this study. All samples were analyzed for their δ26Mg∗ and 27Al/24Mg ratios, in order to construct both whole rock and model whole rock isochrons. Mineral separation was performed on 8 of the HED's in order to obtain internal isochrons. While whole rock Al-Mg analyses of HED's plot on a regression that could be interpreted as a vestan planetary isochron, internal mineral isochrons indicate a more complex history. Crystallization ages obtained from internal 26Al-26Mg systematic in basaltic eucrites show that Vesta's upper crust was formed during a short period of magmatic activity at 2.66-0.58+1.39 million years (Ma) after Calcium-Aluminum inclusions (after CAI). We also suggest that impact metamorphism and subsequent age resetting could have taken place at the surface of Vesta while 26Al was still extant. Cumulate eucrites crystallized progressively from 5.48-0.60+1.56 to >7.25 Ma after CAI. Model ages obtained for both basaltic and cumulate eucrites are similar and suggest that the timing of differentiation of a common eucrite source from a chondritic body can be modeled at 2.88-0.12+0.14 Ma after CAI, i.e. contemporaneously from the onset of the basaltic eucritic crust. Based on their cumulate texture, we suggest cumulate eucrites were likely formed deeper in the crust of Vesta. Diogenites have a more complicated history and their 26Al-26Mg systematics show that they likely formed after the complete decay of 26Al and thus are younger than eucrites. This refined chronology for eucrites and diogenites is consistent with a short magma ocean stage on 4-Vesta from which the basaltic eucrites rapidly crystallized. In order to explain the younger age and the complex history of diogenites, we postulate that a second episode of magmatism was possibly triggered by a mantle overturn. We bring a refined chronology of the geological history of Vesta that shows that the asteroid has known a more-complex differentiation than previously thought.

Vesta is not an intact protoplanet

NASA Astrophysics Data System (ADS)

Consolmagno, G.; Turrini, D.; Golabek, G.; Svetsov, V.; Sirono, S.; Tsiganis, K.

2014-07-01

The Dawn mission was designed to explore ''remnant intact protoplanets from the earliest epoch of solar system formation'' [1]. However, models of Vesta composed of an iron core, olivine mantle, and HED crust in chondritic proportions cannot match the joint constraints from Dawn [1] of Vesta's density, core size, and the extremely limited presence of exposed olivine on its surface. Vesta has a mean density of 3456 kg/m3 and its surface composition is well matched by howardites. The Dawn gravity data suggest a nickel-iron core of radius 110 km and density 7500--7800 kg/m3. The Rheasilvia impact basin, formed within a pre-existing large basin, Veneneia, should have excavated material from a depth of 50 km to 80 km or more below Vesta's surface [2]. If the howardite crust were thinner than 50--80 km, a significant amount of olivine-rich material, derived from depth, would have been exposed within this basin; models suggest that olivine would also be distributed both on Vesta's surface and in space as meteorite-source Vestoids. Such olivine is rare on Vesta, among the Vestoids, or in our meteorite collection. Vesta's density is similar to an L chondrite, but the Na and K abundances in Vesta are strongly depleted compared to chondrites and the average metal content of an L chondrite, 8.4% by mass, would give a core radius less than 90 km. A 110 km radius metallic core, via the Dawn data, represents 15% of Vesta's mass. The Mg/Al ratio in cosmic abundances is about 10:1, but roughly 1:1 within the eucrites; thus if Vesta started with cosmic abundances, the eucrites can only represent 10% of the parent body total mass. Likewise the 10 x chondritic rare earth trace elements (REE) abundance seen in most eucrites demands that, regardless of formation mechanism, these basalts were crystallized from a melt representing 10% of the mass of the source region [3]. Thus the howardite crust of a chondritic HED parent body, mixing all the available eucritic and diogenitic material (in a 2:1 ratio), represents no more than 15% of its total mass. This leaves 70% of Vesta's mass as olivine. Assuming no porosity in this mantle, the radius and density of Vesta can be matched only with a howardite crust (average grain density [4] of 3270 kg/m3) that was 27 km thick with a porosity of nearly 45%, comparable to sand. If the mantle porosity is 8%, similar to Chassigny, the necessary crust porosity would be 30%, but its thickness would drop to 21 km. In both cases, this crust is too thin to accommodate the lack of olivine in Rheasilvia or its ejecta. Absent some unknown process to hide large amounts of olivine on the surface of Vesta and among the Vestoids, chondritic models do not fit the observational constraints. A larger, lower density core of olivine and metal mixed in equal proportions (by mass), of density 5000 kg/m3 and radius 145 km may also fit the Dawn gravity data [5]. The remaining volume of Vesta would be a 115 km thick howardite crust, thick enough to allow the metal/olivine core to remain unexposed. (In this case Vesta would be composed only of core and crust, but the core would be rich in olivine.) To match Vesta's density, this thick crust only needs an average porosity of 4%. Since 50% of Vesta's mass in this model would be eucrites, the REE abundances for the whole of Vesta would have to be five times chondritic values. Either Vesta accreted from a highly unusual cosmochemical setting, or 80% of its primordial olivine and iron were removed at some time after the REE trace elements were extracted from the bulk proto-Vesta into the eucritic melt. This proto-Vesta would have to have at least three times the mass of the current Vesta, with a radius of at least 375 km (still smaller than Ceres). Either Vesta formed with a very non-chondritic composition or it was subjected to a radical change in composition, presumably due to the intense collisional environment [6,7] where and when it formed. In any event, Vesta is not a remnant protoplanet but a chemically stripped and reaccreted body.

Basaltic volcanism - The importance of planet size

NASA Technical Reports Server (NTRS)

Walker, D.; Stolper, E. M.; Hays, J. F.

1979-01-01

The volumetrically abundant basalts on the earth, its moon, and the eucrite parent planet all have chemical compositions that are controlled to a large extent by dry, low-pressure, crystal-liquid equilibria. Since this generalization is valid for these three planetary bodies, we infer that it may also apply to the other unsampled terrestrial planets. Other characteristics of basaltic volcanism show variations which appear to be related to planet size: the eruption temperatures, degrees of fractionation, and chemical variety of basalts and the endurance of basaltic volcanism all increase with planet size. Although the processes responsible for chemical differences between basalt suites are known, no simple systematization of the chemical differences between basalts from planet to planet has emerged.

Overview of Vesta Mineralogy Diversity

NASA Technical Reports Server (NTRS)

DeSanctis, M. C.; Ammannito, E.; Capria, M. T.; Capaccioni, F.; Carraro, F.; Fonte, S.; Frigeri, A.; Magni, G.; Marchi, S.; Palomba, E.;

Non-equilibrium effects on the chemistry of nebular condensates - Implications for the planets and asteroids

NASA Technical Reports Server (NTRS)

Blander, M.

1979-01-01

Kinetic effects, for example nucleation constraints and slow reactions, should have been important in nebular condensation. Consideration of these effects leads to the prediction of pressure-dependent compositions and physical properties of nebular condensates which is consistent with (1) the differences between different classes of chondritic meteorites, (2) some of the differences between planets, and (3) the presence of oxidized iron on the moon and in the eucrite parent body (presumably an asteroid) despite the low abundance of volatiles. Diffusion effects appear to be important for understanding oxygen isotope anomalies in refractory inclusions in Allende. The consideration of kinetic effects leads to more information concerning nebular processes than if equilibrium is assumed.

Spectral characterization of V-type asteroids - I. Space weathering effects and implications for V-type NEAs

NASA Astrophysics Data System (ADS)

Fulvio, Daniele; Perna, Davide; Ieva, Simone; Brunetto, Rosario; Kanuchova, Zuzana; Blanco, Carlo; Strazzulla, Giovanni; Dotto, Elisabetta

2016-01-01

Among main belt asteroids, V-types belonging to Vesta's dynamical family are known as `Vestoids' while those lying outside Vesta's family as `non-Vestoids'. V-types have also been found within the population of Near Earth Asteroids (NEAs). Several questions on Vesta, the V-types, and the Howardite-Eucrite-Diogenite meteorites are still unsolved, such as the genesis of each class/subclass, their evolution and mutual relationship, and the existence of other basaltic parent bodies. We present new NIR (0.8-2.4 μm) spectroscopic observations of seven non-Vestoids, carried out at the Telescopio Nazionale Galileo (TNG - INAF). We derived a number of spectral parameters (BI and BII centres, band separations, and BI slopes) and compared them with available spectra of V-types belonging to different subclasses (102 V-types in total), to highlight possible spectral differences useful to shed light on the questions mentioned above. We also considered the data from ion irradiation experiments performed on different samples of eucrites, simulating space weathering effects. Net discrepancies are seen for the BI slope distributions: NEAs show a distribution strongly different from all other V-type subclasses. Ion irradiation experiments induce strong effects on BI slope values and, as irradiation proceeds, the BI slope of eucrites quickly increases, changing the overall aspect of their VIS-NIR spectra (0.4-2.5 μm). Space weathering may explain the whole range of spectral slopes observed for all V-type subclasses. An exception is represented by NEAs, where moderate space weathering effects are evidenced. We propose that this is due to tidal perturbations exposing `fresh' unweathered surface grains during close encounters with the Earth, as previously found for Q-type NEAs.

A model composition for Mars derived from the oxygen isotopic ratios of martian/SNC meteorites. [Abstract only

NASA Technical Reports Server (NTRS)

Delaney, J. S.

1994-01-01

Oxygen is the most abundant element in most meteorites, yet the ratios of its isotopes are seldom used to constrain the compositional history of achondrites. The two major achondrite groups have O isotope signatures that differ from any plausible chondritic precursors and lie between the ordinary and carbonaceous chondrite domains. If the assumption is made that the present global sampling of chondritic meteorites reflects the variability of O reservoirs at the time of planetessimal/planet aggregation in the early nebula, then the O in these groups must reflect mixing between known chondritic reservoirs. This approach, in combination with constraints based on Fe-Mn-Mg systematics, has been used previously to model the composition of the basaltic achondrite parent body (BAP) and provides a model precursor composition that is generally consistent with previous eucrite parent body (EPB) estimates. The same approach is applied to Mars exploiting the assumption that the SNC and related meteorites sample the martian lithosphere. Model planet and planetesimal compositions can be derived by mixing of known chondritic components using O isotope ratios as the fundamental compositional constraint. The major- and minor-element composition for Mars derived here and that derived previously for the basaltic achondrite parent body are, in many respects, compatible with model compositions generated using completely independent constraints. The role of volatile elements and alkalis in particular remains a major difficulty in applying such models.

Constraints on Vesta's elemental composition: Fast neutron measurements by Dawn's gamma ray and neutron detector

PubMed Central

Lawrence, David J; Peplowski, Patrick N; Prettyman, Thomas H; Feldman, William C; Bazell, David; Mittlefehldt, David W; Reedy, Robert C; Yamashita, Naoyuki

2013-01-01

Surface composition information from Vesta is reported using fast neutron data collected by the gamma ray and neutron detector on the Dawn spacecraft. After correcting for variations due to hydrogen, fast neutrons show a compositional dynamic range and spatial variability that is consistent with variations in average atomic mass from howardite, eucrite, and diogenite (HED) meteorites. These data provide additional compositional evidence that Vesta is the parent body to HED meteorites. A subset of fast neutron data having lower statistical precision show spatial variations that are consistent with a 400 ppm variability in hydrogen concentrations across Vesta and supports the idea that Vesta's hydrogen is due to long-term delivery of carbonaceous chondrite material. PMID:26074718

Geological Structures in the WaIls of Vestan Craters

NASA Technical Reports Server (NTRS)

Mittlefehldt, David; Nathues, A.; Beck, A. W.; Hoffmann, M.; Schaefer, M.; Williams, D. A.

2014-01-01

A compelling case can be made that Vesta is the parent asteroid for the howardite, eucrite and diogenite (HED) meteorites [1], although this interpretation has been questioned [2]. Generalized models for the structure of the crust of Vesta have been developed based on petrologic studies of basaltic eucrites, cumulate eucrites and diogenites. These models use inferred cooling rates for different types of HEDs and compositional variations within the clan to posit that the lower crust is dominantly diogenitic in character, cumulate eucrites occur deep in the upper crust, and basaltic eucrites dominate the higher levels of the upper crust [3-5]. These models lack fine-scale resolution and thus do not allow for detailed predictions of crustal structure. Geophysical models predict dike and sill intrusions ought to be present, but their widths may be quite small [6]. The northern hemisphere of Vesta is heavily cratered, and the southern hemisphere is dominated by two 400-500 km diameter basins that excavated deep into the crust [7-8]. Physical modeling of regolith formation on 300 km diameter asteroids predicts that debris layers would reach a few km in thickness, while on asteroids of Vesta's diameter regolith thicknesses would be less [9]. This agrees well with the estimated =1 km thickness of local debris excavated by a 45 km diameter vestan crater [10]. Large craters and basins may have punched through the regolith/megaregolith and exposed primary vestan crustal structures. We will use Dawn Framing Camera (FC) [11] images and color ratio maps from the High Altitude and Low Altitude Mapping Orbits (HAMO, 65 m/pixel; LAMO, 20 m/pixel) to evaluate structures exposed on the walls of craters: two examples are discussed here.

Geologic History of Asteroid 4 Vesta

NASA Technical Reports Server (NTRS)

Mittlefehldt, David W.

2014-01-01

Some types of meteorites - most irons, stony irons, some achondrites - hail from asteroids that were heated to the point where magmatism occurred within a very few million years of the formation of the earliest solids in the solar system. The largest clan of achondrites, the howardite, eucrite and diogenite (HED) meteorites, represent the crust of their parent asteroid]. Diogenites are cumulate harzburgites and orthopyroxenites from the lower crust whilst eucrites are basalts, diabases and cumulate gabbros from the upper crust. Howardites are impact-engendered breccias mostly of diogenites and eucrites. There remains only one large asteroid with a basaltic crust, 4 Vesta, which is thought to be the source of the HED clan. Differentiation models for Vesta are based on HED compositions. Proto-Vesta consisted of chondritic materials containing Al-26, a potent, short-lived heat source. Inferences from compositional data are that Vesta was melted to high degree (=50%) allowing homogenization of the silicate phase and separation of a metallic core. Convection of the silicate magma ocean allowed equilibrium crystallization, forming a harzburgitic mantle. After convective lockup occurred, melt collected between the mantle and the cool thermal boundary layer and underwent fractional crystallization forming an orthopyroxene-rich (diogenite) lower crust. The initial thermal boundary layer of chondritic material was replaced by a mafic upper crust through impact disruption and foundering. The mafic crust thickened over time as additional residual magma intrudes and penetrates the mafic crust forming plutons, dikes, sills and flows of cumulate and basaltic eucrite composition. This magmatic history may have taken only 2-3 Myr. This magma ocean scenario is at odds with a model of heat and magma transport that indicates that small degrees of melt would be rapidly expelled from source regions, precluding development of a magma ocean. Constraints from radiogenic Mg-26 distibutions suggest that the parent asteroid of HEDs was much smaller than Vesta. Thus, first-order questions regarding asteroid differentiation remain.

Pristine Igneous Rocks and the Early Differentiation of Planetary Materials

NASA Technical Reports Server (NTRS)

Warren, Paul H.

2005-01-01

Our studies are highly interdisciplinary, but are focused on the processes and products of early planetary and asteroidal differentiation, especially the genesis of the ancient lunar crust. The compositional diversity that we explore is the residue of process diversity, which has strong relevance for comparative planetology. Most of the accessible lunar crust consists of materials hybridized by impact-mixing. Our lunar research concentrates on the rare pristine (unmixed) samples that reflect the original genetic diversity of the early crust. Among HED basalts (eucrites and clasts in howardites), we distinguish as pristine the small minority that escaped the pervasive thermal metamorphism of the parent asteroid's crust. We have found a correlation between metamorphically pristine HED basalts and the similarly small minority of compositionally evolved "Stannern trend" samples, which are enriched in incompatible elements and titanium compared to main group eucrites, and yet have relatively high mg ratios. Other topics under investigation included: lunar and SNC (martian?) meteorites; igneous meteorites in general; impact breccias, especially metal-rich Apollo samples and polymict eucrites; siderophile compositions of the lunar and martian mantles; and planetary bulk compositions and origins.

History of the Pasamonte achondrite: Relative susceptibility of the SmNd, RbSr, and UPb systems to metamorphic events

USGS Publications Warehouse

Unruh, D.M.; Nakamura, N.; Tatsumoto, M.

1977-01-01

The RbSr, SmNd, and UPb systematics of the eucrite Pasamonte have been studied in order to investigate the relative susceptibility of the different systems to post-crystallization events and to determine the age and history of the meteorite. The RbSr and 238U-206Pb data of mineral separates do not define an isochron but the SmNd data define an internal isochron which corresponds to the formation age of 4.58 ?? 0.12 b.y. (109 years). The 207Pb-206Pb data of mineral separates define an apparent age of 4.53 ?? 0.03 b.y., however we conclude that this age, while in agreement with the SmNd age, is not strictly valid since the UPb data indicate at least three stages of evolution. The UPb data indicate that the parent body of the meteorite experienced brecciation shortly after the formation of the parent body surface (???4.2-4.45 b.y. ago) and a recent disturbance (collision?) 6 ?? 30 m.y. ago. The latter age is within the range of cosmic ray exposure ages for achondrites. ?? 1977.

Petrology of Zircon-Bearing Diogenite Northwest Africa 10666

NASA Technical Reports Server (NTRS)

Tanner, T. B.; Jeffcoat, C. R.; Righter, M.; Berger, E. L.; Lapen, T. J.; Irving, A. J.; Kuehner, S. M.; Fujihara, G.

2017-01-01

The howardite, eucrite, and diogenite (HED) meteorites are a group of achondrites thought to be derived from the asteroid 4 Vesta, though there is active debate as to whether all diogenites are part of the HED suite. Petrologic investigation of the HED meteorite group provides a means of understanding early planetary differentiation processes and early evolution of planets in our solar system. Diogenites are predominantly coarse grained ortho-pyroxenites with some samples containing appreciable amounts of clinopyroxene, olivine, chromite, and plagioclase. Accessory metal, troilite, and apatite are common. Many diogenites are brecciated, however, there are few poorly to unbrecciated samples. Diogenites are important because they may represent the lower crust of 4 Vesta. Although Mg isotope data indicates that the sources of diogenites are ancient, their crystallization ages are difficult to constrain due to their protracted thermal histories. The limited chronologic data for diogenites also limits the ability to test petrogenetic connections with eucrites and even parent body. A reliable and high closure-temperature isotope system, such as U-Pb in zircon, is needed to address the timing of diogenite igneous crystallization. Description of the textures and mineralogy of diogenites are essential to their classification and understanding their formation, in particular, whether all phases are petrogenetically related. Here, we present detailed petrographic data from a rare zircon-bearing feldspathic diogenite, Northwest Africa (NWA) 10666 and provide textural evidence for igneous crystallization of the zircon.

Comment on "Reconciliation of the excess 176Hf conundrum in meteorites: Recent disturbances of the Lu-Hf and Sm-Nd isotope systematics" [Geochim. Cosmochim. Acta 212 (2017) 303-323

NASA Astrophysics Data System (ADS)

Bloch, Elias; Watkins, James; Ganguly, Jibamitra

2018-06-01

In a recent paper, Bast et al. (2017) present an impressive set of mineral and whole rock isochrons and use them to investigate the cause(s) of excess 176Hf in eucrite and angrite meteorites. They argue that during terrestrial weathering of these samples, phosphates present as isolated grains or inclusions underwent partial dissolution during which Lu was mobilized more effectively than Hf. If this residual, unsupported Hf were not effectively excluded from analyses, then the data points would be shifted above the actual isochron, creating scatter and potentially spurious Lu-Hf ages. Bast et al. (2017) conclude that: (1) diffusive fractionation of Lu from Hf during a thermal metamorphic event on the parent body, as suggested by Bloch et al. (2017) and Debaille et al. (2011), did not contribute significantly to the anomalous Lu-Hf ages, and (2) terrestrial weathering effects are the primary cause of the older-than-solar-system Lu-Hf mineral ages retrieved from some eucrites and angrites (e.g. Bast et al., 2012; Bizzarro et al., 2012; Lapen et al., 2015; Sanborn et al., 2015). We find these conclusions to be unjustified in light of the authors' selective and incomplete consideration of results from the modeling by Bloch et al. (2017).

Core formation in the Moon: The mystery of the excess depletion of Mo, W and P

NASA Technical Reports Server (NTRS)

Newsom, H. E.; Maehr, S. A.

1993-01-01

We have evaluated siderophile element depletion models for the Moon in light of our improved statistical treatment of siderophile element abundance data and new information on the physics of core formation. If core formation occurred in the Moon at the large degrees of partial melting necessary for metal segregation, according to recent estimates, then a significant inconsistency (not seen in the eucrite parent body) exists in the depletion of the incompatible siderophile elements Mo, W, and P, compared to other siderophile elements in the Moon. The siderophile data, with the exception of Mo, are most consistent with terrestrial initial siderophile abundances and segregation of a very small core in the Moon. Our improved abundance estimates and possible explanations for these discrepancies are discussed.

Asteroidal Differentiation - The Record in Meteorites

NASA Technical Reports Server (NTRS)

Mittlefehldt, David W.

2010-01-01

Early in solar system history, an intense energy source modified the small rocky bodies that had accreted from nebular condensates. The consensus view is that this energy source was the decay of short-lived 26Al, perhaps with a contribution from short-lived 60Fe. Differentiated meteorites and primitive achondrites preserve records of the states of asteroids as differentiation was ending. Reading these records provides clues to the nature of the energy source and the mechanisms of differentiation. I will examine the records from the acapulcoite-lordanite clan, ureilites, main-group pallasites, magmatic iron meteorite groups, brachinites and howardite-eucrite-diogenite (HED) clan meteorites. The acapulcoite-lodranite clan and the ureilites contain evidence that their parent asteroids reached temperatures where basaltic melts were produced. The mineralogies of lodranites and ureilites are dominantly olivine and low-Ca pyroxene, and these meteorites are highly depleted in incompatible lithophile elements. The acapulcoite-lodranite and ureilite parent bodies were heated to the point where on the order of 20-30% melting had taken place, but there is no evidence for more extensive melting. Assuming a 26Al energy source, the implication is that transport of the Al-rich basalt out of the mantle outpaced radiogenic heating, and thus shut down further differentiation. Main-group pallasites, magmatic iron meteorites and HED clan meteorites, on the other hand, provide evidence for total or near total melting of asteroids. The silicate phase of pallasites is magnesian olivine; their minor and trace element contents suggest that they are refractory melting residues. The degree of melting was high, perhaps on the order of 80%. The compositions of the most Ir-rich magmatic irons suggest near total melting of the metallic phase, and thus high degrees of melting on their parent asteroids. The compositions of basaltic eucrites are most consistent with them being residues from the crystallization of a largely molten asteroid. For these meteorite groups, the rate of heating outpaced the rate at which the melt could be extracted from the interiors, again, assuming 26Al was the energy source. The nature of the heat engine and asteroidal differentiation processes will be discussed as they can be inferred from the petrology and composition of achondrites, irons and stony irons.

Relationships Between HED's, Mesosiderites, and Ungrouped Achondrites: Trace Element Analyses of Mesosiderite RKPA 79015 and Ungrouped Achondrite QUE 93148

NASA Technical Reports Server (NTRS)

Righter, M.; Lapen, T.; Righter, K.

2008-01-01

Achondritic meteorites are a diverse group of meteorites that formed by igneous activity in asteroids. These meteorites can provide important information about early differentiation processes on asteroidal bodies. The howardite-eucrite-diogenite (HED) meteorites, the largest group of achondrites, are the only group of meteorites for which a potential parent body has been identified (4 Vesta) [e.g., 1]. Mesosiderites are stony-iron meteorites composed of roughly equal amounts of metal and silicates and silicates are broadly similar to HED meteorites [2]. They may have been formed by impact-mixing of crustal and core materials of differentiated meteorite parent bodies. Chemical and oxygen isotopic compositional data suggest that the HED meteorites and silicate portions of mesosiderites originated on the same or closely related parent bodies. Pallasites and IIIAB irons also have similar oxygen isotope compositions and have been thought to be related to the HEDs [3,4]. However, recent high resolution analyses have shown that pallasites and HED's have different oxygen isotopic values, but mesosiderites and HED s have the same isotope compositions implying a close connection [5]. QUE 93148 is a small (1.1g) olivine-rich (mg 86) achondrite that contains variable amounts of orthopyroxenene (mg 87) and kamacite (6.7 wt% Ni), with minor augite [6]. This meteorite was originally classified as a lodranite [7], but it s oxygen isotopic composition precludes a genetic relationship to the acapulcoites and lodranites. And also this meteorite has a lower Mn/Mg ratio than any major group of primitive or evolved achondrites and suggested that QUE 93148 may be a piece of the deep mantle of the HED parent body [6]. To better understand the relationship between HED s, mesosiderites and related achondrites, we have measured trace elements in the individual metallic and silicate phases. In this study, abundances of a suite of elements were measured for the unusual mesosiderite RKPA 79015 and a ungrouped achondrite QUE93148.

Asteroid 4 Vesta: A Fully Differentiated Dwarf Planet

NASA Technical Reports Server (NTRS)

Mittlefehldt, David

2014-01-01

One conclusion derived from the study of meteorites is that some of them - most irons, stony irons, some achondrites - hail from asteroids that were heated to the point where metallic cores and basaltic crusts were formed. Telescopic observations show that there remains only one large asteroid with a basaltic crust, 4 Vesta; present day mean radius 263 km. The largest clan of achondrites, the howardite, eucrite and diogenite (HED) meteorites, represent the crust of their parent asteroid. Diogenites are cumulate harzburgites and orthopyroxenites from the lower crust whilst eucrites are cumulate gabbros, diabases and basalts from the upper crust. Howardites are impact-engendered breccias of diogenites and eucrites. A strong case can be made that HEDs are derived from Vesta. The NASA Dawn spacecraft orbited Vesta for 14 months returning data allowing geological, mineralogical, compositional and geophysical interpretations of Vesta's surface and structure. Combined with geochemical and petrological observations of HED meteorites, differentiation models for Vesta can be developed. Proto-Vesta probably consisted of primitive chondritic materials. Compositional evidence, primarily from basaltic eucrites, indicates that Vesta was melted to high degree (>=50%) which facilitated homogenization of the silicate phase and separation of immiscible Fe,Ni metal plus Fe sulphide into a core. Geophysical models based on Dawn data support a core of 110 km radius. The silicate melt vigorously convected and initially followed a path of equilibrium crystallization forming a harzburgitic mantle, possibly overlying a dunitic restite. Once the fraction of crystals was sufficient to cause convective lockup, the remaining melt collected between the mantle and the cool thermal boundary layer. This melt undergoes fractional crystallization to form a dominantly orthopyroxenite (diogenite) lower crust. The initial thermal boundary layer of primitive chondritic material is gradually replaced by a mafic crust through impact disruption and foundering. The quenched mafic crust thickens over time through magma extrusion/intrusion. Melt from the residual magma ocean intrudes and penetrates the mafic crust forming cumulate eucrite plutons, and dikes, sills and flows of basaltic eucrite composition. The post-differentiation vestan structure is thus not too dissimilar from that of terrestrial planets: (i) a metallic core; (ii) an ultramafic mantle comprised of a lower dunitic layer (if melting was substantially <100%) and an upper cumulate harzburgitic layer; (iii) a lower crust of harzburgitic and orthopyroxenitic cumulates; and (iv) an upper mafic crust of basalts and diabases (melt compositions) with cumulate gabbro intrusions. Impacts have excavated to the lower crust and delivered howardites, eucrites and diogenites to Earth, but there is yet no evidence demonstrating excavation of the vestan mantlle.

Mesosiderites on Vesta: A Hyperspectral VIS-NIR Investigation

NASA Technical Reports Server (NTRS)

Palomba, E.; Longobardo, A.; DeSanctis, M. C.; Mittlefehldt, D. W.; Ammannito, E.; Capaccioni, F.; Capria, M. T.; Frigeri, A.; Tosi, F.; Zambon, F.;

The differentiation of eucrites: The role of in situ crystallization

NASA Astrophysics Data System (ADS)

Barrat, J. A.; Blichert-Toft, J.; Gillet, Ph.; Keller, F.

2000-09-01

We report on major and trace element analyses of 17 eucrites, including three cumulate eucrites (Binda, Moore County, and Serra de Magé), determined by, respectively, ICP-AES and ICP-MS. The results obtained for Binda and Moore County are consistent with the model of Treiman (1997) for the formation of cumulate eucrites, which holds that these meteorites were produced from a eucritic melt. Our sample of Serra de Magé contains unusually large amounts of pyroxene and probably an accessory phase rich in HREEs and is therefore not representative of this eucrite as known from literature data. Our results for the noncumulate eucrites Bereba, Bouvante, Cachari, Caldera, Camel Donga, Ibitira, Jonzac, Juvinas, Lakangaon, Millbillillie, Padvarninkai, Pasamonte, Sioux County and Stannern are in good agreement with literature data. The observed decoupling between major and trace elements for noncumulate eucrites can be explained by in-situ crystallization during the differentiation of an asteroidal magma ocean. This model can further account for both the Nuevo Laredo and the Stannern trends but has as a consequence that none of the analyzed eucrites represents a primary melt.

Chemical composition of Mars

NASA Technical Reports Server (NTRS)

Morgan, J. W.; Anders, E.

1979-01-01

The chemical composition of Mars is estimated from the cosmochemical model of Ganapathy and Anders (1974) with additional petrological and geophysical constraints. The model assumes that planets and chondrites underwent the same fractionation processes in the solar nebula, and constraints are imposed by the abundance of the heat-producing elements, U, Th and K, the volatile-rich component and the high density of the mantle. Global abundances of 83 elements are presented, and it is noted that the mantle is an iron-rich garnet wehrlite, nearly identical to the bulk moon composition of Morgan at al. (1978) and that the core is sulfur poor (3.5% S). The comparison of model compositions for the earth, Venus, Mars, the moon and a eucrite parent body suggests that volatile depletion correlates mainly with size rather than with radial distance from the sun.

Pigeonholing planetary meteorites: The lessons of misclassification of EET87521 and ALH84001

NASA Technical Reports Server (NTRS)

Lindstrom, M. M.; Treiman, A. H.; Mittlefehldt, D. W.

1994-01-01

The last few years have provided two noteworthy examples of misclassifications of achondritic meteorites because the samples were new kinds of meteorites from planetary rather than asteroidal parent bodies. Basaltic lunar meteorite EET87521 was misclassified as a eucrite and SNC (martian) orthopyroxenite ALH84001 was misclassified as a diogenite. In classifying meteorites we find what we expect: we pigeonhole meteorites into known categories most of which were derived from the more common asteroidal meteorites. But the examples of EET8752 and ALH84001 remind us that planets are more complex than asteroids and exhibit a wider variety of rock types. We should expect variety in planetary meteorites and we need to know how to recognize them when we have them. Our intent here is to show that our asteroidal perspective is inappropriate for planetary meteorites.

Siderophile Element Depletion in the Angrite Parent Body (APB) Mantle: Due to Core Formation?

NASA Technical Reports Server (NTRS)

Righter, K.

2008-01-01

The origin of angrites has evaded scientists due in part to unusual mineralogy, oxidized character, and small numbers of samples. Increased interest in the origin of angrites has stemmed from the recovery of approximately 10 new angrites in the past decade. These new samples have allowed meteoriticists to recognize that angrites are compositionally diverse, old, and record very early differentiation. Also, a magma ocean has been proposed to have been involved in APB early differentiation, but this remains untested for siderophile elements which are commonly cited as one of the main lines of evidence for magma oceans on the early Earth, Moon, Mars and eucrite parent body (e.g., [6]). And recent suggestions that angrites may or may not be from Mercury have also peaked interest in these achondrites. Given all of this background, a detailed understanding of the early differentiation process is desired. Previous efforts at examining siderophile element (SE) concentrations with respect to core formation processes in the APB have not resulted in any definite conclusions regarding segregation of a metallic core. The goal of this study is to summarize what is known about SE concentrations in the suite, estimate depletions of SE compared to chondrites, and apply metal/silicate experimental partition coefficients to assess whether the APB had a core.

Isotopic, Chemical and Mineralogical Investigation's of Extraterrestrial Materials

NASA Technical Reports Server (NTRS)

Lugmair, G. W.

2003-01-01

During the grant period we have concentrated on the following main topics: 1. Enstatite meteorites and original heterogeneity of Mn-53 distribution in the solar nebula. We have completed our studies of the enstatite chondrites. 2. Processes of planetary differentiation. We have completed our study of silicate clasts from the mesosiderite Vaca Muerta and found that the global Mn/Cr fractionation event that established mantle source reservoirs on the parent body of the Vaca Muerta silicate clasts occurred approx. 2 Ma after a similar event on the howardite-eucrite-diogenite (HED) parent body. 3. Carbonaceous chondrites. Much effort has been devoted during the last three years to the investigation of this important class of meteorites. 4. Early solar system timescales. Based on the studies of the Mn-53 - Cr-53 isotope system in various meteorites and using results obtained with other isotope chronometers we constructed an absolute time-scale for events in the early solar system. 5.Unusual meteorites. We have studied the anomalous pallasite Eagle Station. 6. The chromium isotopic composition as a tracer for extraterrestrial material on Earth. Based on the observed difference in the Cr-53/Cr-52 ratios between Earth and the other solar system objects we developed a method for detecting cosmic materials on Earth using the Cr-53/Cr-52 ratio as a tracer.

Igneous fractionation and subsolidus equilibration of diogenite meteorites

NASA Technical Reports Server (NTRS)

Mittlefehldt, David W.

1993-01-01

Diogenites are coarse-grained orthopyroxenite breccias of remarkably uniform major element composition. Most diogenites contain homogeneous pyroxene fragments up to 5 cm across of Wo2En74Fs24 composition. Common minor constituents are chromite, olivine, trolite and metal, while silica, plagioclase, merrillite and diopside are trace phases. Diogenites are generally believed to be cumulates from the eucrite parent body, although their relationship with eucrites remains obscure. It has been suggested that some diogenites are residues after partial melting. I have performed EMPA and INAA for major, minor and trace elements on most diogenites, concentrating on coarse-grained mineral and lithic clasts in order to elucidate their igneous formation and subsequent metamorphic history. Major element compositions of diogenites are decoupled from minor and trace element compositions; the latter record an igneous fractionation sequence that is not preserved in the former. Low equilibration temperatures indicate that major element diffusion continued long after crystallization. Diffusion coefficients for trivalent and tetravalent elements in pyroxene are lower than those of divalent elements. Therefore, major element compositions of diogenites may represent means of unknown portions of a cumulate homogenized by diffusion, while minor and trace elements still yield information on their igneous history. The scale of major element equilibration is unknown, but is likely to be on the order of a few cm. Therefore, the diogenite precursors may have consisted largely of cm-sized, igneously zoned orthopyroxene grains, which were subsequently annealed during slow cooling, obliterating major element zoning but preserving minor and trace incompatible element zoning.

Micrometer-scale U-Pb age domains in eucrite zircons, impact re-setting, and the thermal history of the HED parent body

NASA Astrophysics Data System (ADS)

Hopkins, M. D.; Mojzsis, S. J.; Bottke, W. F.; Abramov, O.

2015-01-01

Meteoritic zircons are rare, but some are documented to occur in asteroidal meteorites, including those of the howardite-eucrite-diogenite (HED) achondrite clan (Rubin, A. [1997]. Meteorit. Planet. Sci. 32, 231-247). The HEDs are widely considered to originate from the Asteroid 4 Vesta. Vesta and the other large main belt asteroids record an early bombardment history. To explore this record, we describe sub-micrometer distributions of trace elements (U, Th) and 235,238U-207,206Pb ages from four zircons (>7-40 μm ∅) separated from bulk samples of the brecciated eucrite Millbillillie. Ultra-high resolution (∼100 nm) ion microprobe depth profiles reveal different zircon age domains correlative to mineral chemistry and to possible impact scenarios. Our new U-Pb zircon geochronology shows that Vesta's crust solidified within a few million years of Solar System formation (4561 ± 13 Ma), in good agreement with previous work (e.g. Carlson, R.W., Lugmair, G.W. [2000]. Timescales of planetesimal formation and differentiation based on extinct and extant radioisotopes. In: Canup, R., Righter, K. (Eds.), Origin of the Earth and Moon. University of Arizona Press, Tucson, pp. 25-44). Younger zircon age domains (ca. 4530 Ma) also record crustal processes, but these are interpreted to be exogenous because they are well after the effective extinction of 26Al (t1/2 = 0.72 Myr). An origin via impact-resetting was evaluated with a suite of analytical impact models. Output shows that if a single impactor was responsible for the ca. 4530 Ma zircon ages, it had to have been ⩾10 km in diameter and at high enough velocity (>5 km s-1) to account for the thermal field required to re-set U-Pb ages. Such an impact would have penetrated at least 10 km into Vesta's crust. Later events at ca. 4200 Ma are documented in HED apatite 235,238U-207,206Pb ages (Zhou, Q. et al. [2011]. Early basaltic volcanism and Late Heavy Bombardment on Vesta: U-Pb ages of small zircons and phosphates in eucrites. Lunar Planet. Sci. 42. Abstract #2575) and 40-39Ar age spectra (Bogard, D.D. [2011]. Chem. Erde 71, 207-226). Yet younger ages, including those coincident with the Late Heavy Bombardment (LHB; ca. 3900 Ma), are absent from Millbillillie zircon. This is attributable to primordial changes to the velocity distributions of impactors in the asteroid belt, and differences in mineral closure temperatures (Tc zircon ≫ apatite).

Composition and petrology of HED polymict breccias: The regolith of (4) Vesta

NASA Astrophysics Data System (ADS)

Mittlefehldt, David W.; Herrin, Jason S.; Quinn, Julie E.; Mertzman, Stanley A.; Cartwright, Julia A.; Mertzman, Karen R.; Peng, Zhan X.

2013-11-01

We have done petrologic and compositional studies on a suite of polymict eucrites and howardites to better understand regolith processes on their parent asteroid, which we accept is (4) Vesta. Taking into account noble gas results from companion studies, we interpret five howardites to represent breccias assembled from the true regolith: Elephant Moraine (EET) 87513, Grosvenor Mountains (GRO) 95535, GRO 95602, Lewis Cliff (LEW) 85313, and Meteorite Hills (MET) 00423. We suggest that EET 87503 is paired with EET 87513, and thus is also regolithic. Pecora Escarpment (PCA) 02066 is dominated by melt-matrix clasts, which may have been formed from true regolith by impact melting. These meteorites display a range in eucrite:diogenite mixing ratio from 55:45 to 76:24. There is no correlation between degree of regolith character and Ni content. The Ni contents of howardite, eucrite, and diogenites (HEDs) are mostly controlled by the distribution of coarse chondritic clasts and metal grains, which in some cases resulted from individual, low-velocity accretion events, rather than extensive regolith gardening. Trace element compositions indicate that the mafic component of HED polymict breccias is mostly basalt similar to main-group eucrites; Stannern-trend basaltic debris is less common. Pyroxene compositions show that some trace element-rich howardites contain abundant debris from evolved basalts, and that cumulate gabbro debris is present in some breccias. The scale of heterogeneity varies considerably; regolithic howardite EET 87513 is more homogeneous than fragmental howardite Queen Alexandra Range (QUE) 97001. Individual samples of a given howardite can have different compositions even at roughly 5 g masses, indicating that obtaining representative meteorite compositions requires multiple or large samples.

Angrites: A Volatile-rich Variety of Asteroidal Basalt (Except for Alkalis and Gallium!)

NASA Astrophysics Data System (ADS)

Warren, P. H.; Kallemeyn, G. W.

1995-09-01

Angrites are commonly viewed as extremely volatile-depleted, and a related notion is that they formed by differentiation of a very CAI-rich material [e.g., 1]. Partial melting experiments reportedly reproduce the bulk compositions (although not fassaite-rich mineralogy) of angrites with Allende as starting material [2], but highly CAI-rich parent materials are difficult to reconcile with isotopic and REE data [3,4]. Mittlefehldt and Lindstrom [5] inferred from the low Na/Al ratios of angrites that outgassing, and thus primordial magmatism, was more intense on their parent body than on the eucrite parent asteroid. Of seven elements that (a) have been adequately determined in angrites, and (b) are far more volatile (solar-nebula 50% condensation T [6] = 690-430 K) than the alkalis (1000-910 K), four are enriched, and none is significantly depleted, in average angrite compared to average eucrite or low-Ti mare basalt (Figure). Gallium, which is of intermediate volatility (830 K), is depleted to roughly the same extent as Na and K. Results for A881371 [3] are incomplete (Zn, 6 micrograms/g, is near INAA detection limit), but even based only on AdoR and the two LEW angrites, this pattern seems firmly established. Apparent gas cavities in A881371 [7] also suggest that volatiles are far from uniformly depleted. The only elements known to be depleted, as volatiles, by clearly significant factors in angrites versus eucrites or lunar basalts, are alkalis plus gallium. Besides being moderately volatile, a noteworthy characteristic shared among Ga and alkalis (and not shared with elements such as Br, Se, and Zn) is that these elements probably tend to partition into crustal feldspar during gross differentiation of small (low-pressure) bodies. If gallium + alkalis were depleted by a single process starting from "normal" chondritic material, that process would seem to require selective exposure of a feldspar-enriched region (i.e., crust) to extremely high temperature. Igneous crystallization of the angrites occurred when the solar system was still extremely young, and apparently <=2 Ma after the volatile-depletion process [4]. The data of [4] eliminate 26Al as a potential heat source for magmatism. The angrite volatile pattern may be the product of heating by an intense, short-lived heat source that melted and partially vaporized the crust of an asteroid(s) (not necessarily the final angrite asteroid), without much affecting the deep interior(s), which later (through mixing and/or magmatism) replenished the angritic materials in most volatiles, but not alkalis and Ga. Exogenic heating, as in the often-conjectured (but hard to test) hypothesis that a major early heat source was enhanced solar luminosity (as in FU-Orionis cycles), would seem to be required. LEW 87051 and A881371 are rich in compositionally diverse olivine xenocrysts, and A881371 contains a possible FeS xenocryst [7]. These, and the angrites' great siderophile diversity [3], tend to suggest that magmatism and intensely disruptive cratering (with mixing of precursor materials) were contemporaneous. This scenario is admittedly speculative, but the volatile-depletion pattern is difficult to rationalize with any other model. References: [1] Prinz M. and Weisberg M. (1995) Antarct. Meteorites, XX, 207-210. [2] Jurewicz A. et al. (1993) GCA, 57, 2123-2139. [3] Warren P. et al. (1995) Antarct. Meteorites, XX, 261-264. [4] Lugmair G. and Galer S. 1992) GCA, 56, 1673-1694. [5] Mittlefehldt D. and Lindstrom M. (1990) GCA, 54, 3209-3218. [6] Wasson J. (1985) Meteorites. [7] Warren P. and Davis A. (1995) Antarct. Meteorites, XX, 257-260.

Petrography and Origin of the Unique Achondrite GRA 06128 and 06129: Preliminary Results

NASA Technical Reports Server (NTRS)

Treiman, A. H.; Morris, R. V.; Kring, D. A.; Mittlefehldt, D. W.; Jones, J. H.

2008-01-01

GRA 06128 & 06129 are paired achondrites [1], with unique mineral proportions (75% oligoclase), mineral compositions, and oxygen isotope ratios. They appear to represent alkalic igneous rock from a hitherto unsampled differentiated parent body, modified significantly by thermal and shock metamorphism. Samples and Methods: Bulk samples were examined at JSC during splitting for consortium analyses. Microscope and BSE images here are on thick section GRA06128,40. Chemical analyses of minerals were acquired at Johnson Space Center with the Cameca SX100, operated at 15 kV. Feldspar was analyzed with a defocused 5 micron beam @ 5 nA; other minerals were analyzed with a focused beam @ 20 nA. Moessbauer spectra were obtained at ARES, JSC [2]. Intrinsic radioactivity was measured in the low-level counting facility at ARES JSC [3]. An estimated abundance of Al-26 of approx. 70 dpm/kg is within the range determined for eucrites.

Early Thermal History of Eucrites by Ar-39-Ar-40

NASA Technical Reports Server (NTRS)

Bogard, D. D.; Garrison, D. H.

2001-01-01

Ar-39-Ar-40 ages for Piplia Kalan (3.58 +/- 0.02 Ga) and two other eucrites indicate later impact resetting. Older Ar-39-Ar-40 ages exist for the Moama cumulate eucrite (4.42 +/- 0.01 Ga) and the PCA82502 (4.506 +/- 0.009 Ga) and PCA91007 non-brecciated eucrites. Additional information is contained in the original extended abstract.

V, Cr, and Mn in the Earth, Moon, EPB, and SPB and the origin of the Moon: Experimental studies

DOE Office of Scientific and Technical Information (OSTI.GOV)

Drake, M.J.; Capobianco, C.J.; Newsom, H.E.

1989-08-01

The abundances of V, Cr, and Mn inferred for the mantles of the Earth and Moon decrease in that order and are similar, but are distinct from those inferred for the mantles of the Eucrite Parent Body (EPB) and Shergottite Parent Body (SPB). This similarity between Earth and Moon has been used to suggest that the Moon is derived substantially or entirely from Earth mantle material following terrestrial core formation. To test this hypothesis, the authors have determined the partitioning of V, Cr, and Mn between solid iron metal, S-rich metallic liquid, and synthetic basaltic silicate liquid at 1,260{degree}C andmore » one bar pressure. The sequence of compatibility in the metallic phases is Cr > V > Mn at high oxygen fugacity and V > Cr > Mn at low oxygen fugacities. Solubilities in liquid metal always exceed solubilities in solid metal. These partition coefficients suggest that the abundances of V, Cr, and Mn do not reflect core formation in the Earth. Rather, they are consistent with the relative volatilities of these elements. The similarity in the depletion patterns of V, Cr, and Mn inferred for the mantles of the Earth and Moon is a necessary, but not sufficient, condition for the Moon to have been derived wholly or in part from the Earth's mantle.« less

Partial melting of ordinary chondrites: Lost City (H) and St. Severin (LL)

NASA Technical Reports Server (NTRS)

Jurewicz, Amy J. G.; Jones, John H.; Weber, Egon T.; Mittlefehldt, David W.

1993-01-01

Eucrites and diogenites are examples of asteroidal basalts and orthopyroxenites, respectively. As they are found intermingled in howardites, which are inferred to be regolith breccias, eucrites and diogenites are thought to be genetically related. But the details of this relationship and of their individual origins remain controversial. Work by Jurewicz et al. showed that 1170-1180 C partial melts of the (anhydrous) Murchison (CM) chondrite have major element compositions extremely similar to primitive eucrites, such as Sioux County. However, the MnO contents of these melts were about half that of Sioux County, a problem for the simple partial melting model. In addition, partial melting of Murchison could not produce diogenites, because residual pyroxenes in the Murchison experiments were too Fe- and Ca-rich and were minor phases at all but the lowest temperatures. A parent magma for diogenites needs an expanded low-calcium pyroxene field. In their partial melting study of an L6 chondrite, Kushiro and Mysen found that ordinary chondrites did have an expanded low-Ca pyroxene field over that of CV chondrites (i.e., Allende), probably because ordinary chondrites have lower Mg/Si ratios. This study expands that of both Kushiro and Mysen and Jurewicz et al. to the Lost City (H) and St. Severin (LL) chondrites at temperatures ranging from 1170 to 1325 C, at an fO2 of one log unit below the iron-wuestite buffer (IW-1).

Trace Element Abundances in Eucrite Basalts: Enrichment or Depletion?

NASA Astrophysics Data System (ADS)

Castle, N. R.

2018-05-01

It is not clear how incompatible trace element (ITE) variation in eucrite basalts originated. Here, mechanisms for relative ITE enrichment or depletion are experimentally evaluated in an attempt to reconcile the Stannern and main group eucrites.

Petrology of the Indian Eucrite Piplia Kalan

NASA Technical Reports Server (NTRS)

Buchanan, Paul C.; Mittlefehldt, D. W.; Hutchinson, R.; Koeberl, C.; Lindstrom, D. J.; Pandit, M. K.

1999-01-01

Piplia Kalan is an equilibrated eucrite consisting of 60-80 vol.% lithic clasts in a subordinate brecciated matrix. Ophitic/subophitic lithic clasts fall into two groups: finer-grained lithology A and coarser-grained lithology B. Very fine-grained clasts (lithology C) also occur and originally were hypocrystalline in texture. The variety of materials represented in Piplia Kalan suggests cooling histories ranging from quenching or fast crystallization to slower crystallization. Despite textural differences, clasts and matrix have similar mineral and bulk compositions. Thus. Piplia Kalan is probably best classified as a genomict breccia that could represent fragments of a single lava flow or shallow intrusive body, including fine-grained or glassy outer margin and more slowly cooled coarser-grained interior. Piplia Kalan displays evidence of an early shock event, including brecciated matrix and areas of lithic clasts that contain fine-grained, equigranular pyroxene between deformed feldspar laths. The meteorite also displays evidence of at least one episode of thermal metamorphism: hypocrystalline materials are recrystallized to hornfelsic textures and the matrix has a nonporous texture similar to those of eucrites that were affected by post-brecciation heating. Veins of brown glass transect both lithic clasts and brecciated matrix and indicate a second, post-metamorphism shock event.

Predicting the Mineralogy of the HEDs and Vesta Using Both Meteoritic and Synthetic Samples

NASA Astrophysics Data System (ADS)

Mayne, R. G.; Lehman, K.

2012-12-01

Sample return missions are often viewed as the holy grail for planetary science. They enable us to directly correlate samples from the surface of their parent body with spacecraft data, greatly advancing our understanding of the relationship between the petrology and mineralogy of extraterrestrial materials and their corresponding spectra. The link between the Howardite-Eucrite-Diogenite (HED) group of meteorites and the asteroid Vesta provides us with one of the best opportunities for joint petrologic and spectral studies of an airless body. The HEDs can be seen as examples of many "natural" sample return missions. Terrestrial based studies of the HEDs can lead to improved data return from the Dawn mission, currently orbiting and analyzing Vesta. Pyroxenes dominate the HED spectra in the VISNIR region and, consequently, are the primary mineral that will be detected by the VIR instrument aboard Dawn. Previous studies have shown the importance of the high-Ca to low-Ca pyroxene ratio in spectral studies of asteroids, HCP/(HCP+LCP), hereafter referred to as HCP:LCP (Sunshine et al., 2004). This ratio is one of the few petrologic factors that can be predicted from VISNIR spectra and it can be used to indicate the amount of igneous differentiation that the measured surface or sample has undergone (Sunshine et al., 2004). The Modified Gaussian Model (Sunshine et al., 1990) allows to predict the HCP:LCP from spectra. The initial calibrations have been shown in several studies to predict the amount of HCP relative to LCP to within ±5-10 % (Sunshine and Pieters, 1993; Kanner et al., 2007), but for the eucrites this value was ±17 % (Mayne et al., 2010). This is likely because the current calibration for HCP:LCP was calculated using terrestrial composition pyroxene mixtures. The aim of this study is to improve current HCP:LCP calibrations for the HEDs and Vesta by using more Fe-rich, HED-like pyroxene compositions. Two eucrite composition end-member pyroxenes were synthesized by Donald Lindsley at SUNY-Stonybrook using the methods described in Turnock et al. (1973). The composition of the low- and high-Ca synthesized pyroxenes were Wo3.3En35.3Fs61.4 and Wo37.6En29.4Fs33.0 respectively. The pyroxenes were ground in an agate mortar and pestle and <45 μm powders were produced. These powders will be combined to produce a series of known mixtures: 100HCP; 75HCP:25LPC; 50HCP:50LCP; 25HCP:75LCP; 100LCP. The VISNIR (0.32-2.55 μm) spectra of each of these mixtures will be measured using the bidirectional reflectance spectrometer at the NASA/Keck Reflectance Equipment Laboratory (RELAB) at Brown University. The mixture spectra will be analyzed using MGM, with an aim of producing a calibration that allows the HCP:LCP to be accurately predicted for HED meteorites and Vesta. This calibration will be tested on eucrite spectra with a known HCP:LCP ratio from Mayne et al. (2010).

K/TH in Achondrites and Interpretation of Grand Data for the Dawn Mission

NASA Technical Reports Server (NTRS)

Usui, T.; McSween, H. Y., Jr.; Mittlefehldt, D. W.; Prettyman, T. H.

2008-01-01

The Dawn mission will explore 4 Vesta [1], a highly differentiated asteroid believed to be the parent body of the howardite, eucrite and diogenite (HED) meteorite suite [e.g. 2]. The Dawn spacecraft is equipped with a gamma-ray and neutron detector (GRaND), which will enable measurement and mapping of elemental abundances on Vesta s surface [3]. Drawing on HED geochemistry, Usui and McSween [4] proposed a linear mixing model for interpretation of GRaND data. However, the HED suite is not the only achondrite suite representing asteroidal basaltic crusts; others include the mesosiderites, angrites, NWA 011, and possibly Ibitira, each of which is thought to have a distinct parental asteroid [5]. Here we critically examine the variability of GRaND-analyzed elements, K and Th, in HED meteorites, and propose a method based on the K-Th systematics to distinguish between HED and the other differentiated achondrites. Maps of these elements might also recognize incompatible element enriched areas such as mapped locally on the Moon (KREEP) [6], and variations in K/Th ratios might indicate impact volatilization of K. We also propose a new mixing model using elements that will be most reliably measured by GRaND, including K.

Dar Al Gani 872: Yet Another Eucrite, Yet Another Lesson to Learn?

NASA Technical Reports Server (NTRS)

Patzer, A.; Hill, D. H.; Boynton, W. V.; Sipiera, P. P.; Jerman, G. A.

2002-01-01

We present chemical and mineralogical data on a new monomict basaltic eucrite recovered from Libya. In contrast to most other eucrites, it exhibits high shock features, unusually heterogeneous exsolution of pigeonite, and interesting melt pockets. Additional information is contained in the original extended abstract.

The volatile content of Vesta: Clues from apatite in eucrites

NASA Astrophysics Data System (ADS)

Sarafian, Adam Robert; Roden, Michael F.; PatiñO-Douce, Alberto E.

2013-11-01

Apatite was analyzed by electron microprobe in 3 cumulate and 10 basaltic eucrites. Eucritic apatite is fluorine-rich with minor chlorine and hydroxyl (calculated by difference). We confirmed the hydroxyl content by measuring hydroxyl directly in apatites from three representative eucrites using secondary ionization mass spectroscopy. Overall, most eucritic apatites resemble fluorine-rich lunar mare apatites, but intriguing OH- and Cl-rich apatites suggest a role for water and/or hydrothermal fluids in the Vestan interior or on other related differentiated asteroids. Most late-stage apatite found in mesostasis has little hydroxyl or chlorine and is thought to have crystallized from a degassed magma; however, several apatites exhibit atypical compositions and/or textural characteristics. For example, the isotopically anomalous basaltic eucrite Pasamonte has apatite in the mesostasis with significant OH. Apatites in Juvinas also have significant OH and occur as veinlets crosscutting silicates. Euhedral apatites in the Moore County cumulate eucrite occur as inclusions in pyroxene and are also hydroxyl-rich (0.62 wt% OH). The OH was confirmed by SIMS analysis and this apatite clearly points to the presence of water, at least locally, in the Vestan interior. Portions of Elephant Moraine (EET) 90020 have large and abundant apatites, which may be the product of apatite accumulation in a zone of melt-rock reaction. Relatively chlorine-rich apatites occur in basaltic eucrite Graves Nunataks (GRA) 98098 (approximately 1 wt% Cl). Particularly striking is the compositional similarity between apatite in GRA 98098 and apatites in lunar KREEP, which may indicate the presence of residual magmas from an asteroid-wide magma ocean on Vesta.

Characterization of Mineralogy Across Vesta

NASA Technical Reports Server (NTRS)

De Sanctis, M. C.; Ammannito, E.; Capria, M. T.; Capaccioni, F.; Carraro, F.; Fonte, S.; Frigeri, A.; Magni, G.; Marchi, S.; Palomba, E.;

Achondrite Binda; Ordinary Eucrite or the Only Crystalline Howardite?

NASA Astrophysics Data System (ADS)

Yanai, K.

1996-03-01

Binda meteorite, originally classified as howardite (Hey, 1966), was reclassified as eucrite of monomict breccia (Duke and Silver, 1967). Binda was recognized as the most Mg-rich eucrite (or most Fe-rich diogenite) with crystalline-unbrecciated texture for long time. Therefore Binda is believed to have genetic significance in relation to eucrites and diogenites, because in howardite group Binda is the only specimen with unbrecciated or monomict and crystalline texture. Re-examination of Binda was carried out by EPMA, microscope analysis and wet chemical analysis. Binda is the most common (ordinary) encrite showing crystalline texture with slightly brecciated.

Petrologic and Oxygen-Isotopic Investigations of Eucritic and Anomalous Mafic Achondrites

NASA Technical Reports Server (NTRS)

Mittlefehldt, D. W.; Greenwood, R. C.; Peng, Z. X.; Ross, D. K.; Berger, E. L.; Barrett, T. J.

2016-01-01

The most common asteroidal igneous meteorites are eucrite-type basalts and gabbros rocks composed of ferroan pigeonite and augite, calcic plagioclase, silica, ilmenite, troilite, Ca-phosphate, chromite and Fe-metal. These rocks are thought to have formed on a single asteroid along with howardites and diogenites (HEDs). However, Northwest Africa (NWA) 011 is mineralogically identical to eucrites, but has an O-isotopic composition distinct from them and was derived from a different asteroid. Modern analyses with higher precision have shown that some eucrites have smaller O-isotopic differences that are nevertheless well-resolved from the group mean.

Enstatite Meteorites and the Original Heterogeneity of Mn-53 Distribution in the Solar Nebula

NASA Technical Reports Server (NTRS)

Lugmair, Guenter W.

1999-01-01

We have shown earlier that the relative abundance of radiogenic Cr-53 in bulk ordinary chondrites (approximately 0.48 epsilon) is clearly different from that in the earth-moon system (0 epsilon). The SNC parent body (Mars) is characterized by an intermediate Cr-53 excess (approximately 0.23 epsilon). We have also shown that the Mn-Cr systematics of the howardite-eucrite-diogenite parent body (HED PB, the asteroid Vesta) is consistent with the chondritic Mn/Cr ratio in the bulk HED PB and that it has a Cr-53 excess of approximately 0.5 epsilon units which is within error the same as that of chondrites. It appears that the excesses of Cr-53 in these planets are a function of their present heliocentric distance. The study of some other meteorite classes (angrites, pallasites, primitive achondrites) has shown that their Mn-CR systematics is consistent with that of the ordinary chondrites. The observed gradient in the radiogenic Cr-53 abundances can be explained by a). an early volatility controlled radial Mn/Cr fractionation in the nebula or b). an original heterogeneity of Mn-53. The first assumption, however, requires the Mn/Cr ratios of the bulk Earth and Mars to be considerably lower than the inferred model Mn/Cr ratios for these two planets. For this reason, we suggested that the observed gradient is due to an original radial Mn-53 heterogeneity in the late nebula.

High-pressure minerals in shocked meteorites

NASA Astrophysics Data System (ADS)

Tomioka, Naotaka; Miyahara, Masaaki

2017-09-01

Heavily shocked meteorites contain various types of high-pressure polymorphs of major minerals (olivine, pyroxene, feldspar, and quartz) and accessory minerals (chromite and Ca phosphate). These high-pressure minerals are micron to submicron sized and occur within and in the vicinity of shock-induced melt veins and melt pockets in chondrites and lunar, howardite-eucrite-diogenite (HED), and Martian meteorites. Their occurrence suggests two types of formation mechanisms (1) solid-state high-pressure transformation of the host-rock minerals into monomineralic polycrystalline aggregates, and (2) crystallization of chondritic or monomineralic melts under high pressure. Based on experimentally determined phase relations, their formation pressures are limited to the pressure range up to 25 GPa. Textural, crystallographic, and chemical characteristics of high-pressure minerals provide clues about the impact events of meteorite parent bodies, including their size and mutual collision velocities and about the mineralogy of deep planetary interiors. The aim of this article is to review and summarize the findings on natural high-pressure minerals in shocked meteorites that have been reported over the past 50 years.

Experimental determination of the partitioning of gallium between solid iron metal and synthetic basaltic melt Electron and ion microprobe study

NASA Technical Reports Server (NTRS)

Drake, M. J.; Newsom, H. E.; Reed, S. J. B.; Enright, M. C.

1984-01-01

The distribution of Ga between solid Fe metal and synthetic basaltic melt is investigated experimentally at temperatures of 1190 and 1330 C, and over a narrow range of oxygen fugacities. Metal-silicate reversal experiments were conducted, indicating a close approach to equilibrium. The analysis of the partitioned products was performed using electron and ion microprobes. At one bar total pressure, the solid metal/silicate melt partition coefficient D(Ga) is used to evaluate metal-silicate fractionation processes in the earth, moon, and Eucrite Parent Body (EPB). It is found that the depletion of Ga abundances in the EPB is due to the extraction of Ga into a metallic core. Likewise, the depletion of Ga in the lunar mantle is consistent with the extraction of Ga into a smaller lunar core if Ga was originally present in a subchondritic concentration. The relatively high Ga abundances in the earth's mantle are discussed, with reference to several theoretical models.

Getting to Know Vesta

NASA Astrophysics Data System (ADS)

Martel, L. M. V.

2007-11-01

The howardite-eucrite-diogenite class of meteorites (called the HEDs) are rocks formed from basaltic magmas. What makes them special is that the HEDs have reflectance spectra in the visible and near-infrared that match spectra from asteroid 4 Vesta, implying Vesta is their parent body. We will soon have new data from Vesta from NASA's Dawn orbiting spacecraft, which carries a gamma ray and neutron detector, dubbed the GRaND instrument. GRaND will orbit asteroid 4 Vesta and dwarf planet Ceres and map the near-surface abundances of major and minor elements, and volatiles found in ices (in the case of Ceres) such as hydrogen, carbon, nitrogen, and oxygen. Tomohiro Usui and Harry Y. (Hap) McSween, Jr. (University of Tennessee) have proposed a way to interpret the upcoming GRaND data from Vesta based on well-analyzed samples of HED meteorites and a mixing model they devised that uses element ratios of the three expected rock types. In turn, the new data from Vesta may help scientists better understand the geologic context for HED meteorites.

The petrology and chronology of NWA 8009 impact melt breccia: Implication for early thermal and impact histories of Vesta

NASA Astrophysics Data System (ADS)

Liao, Shiyong; Hsu, Weibiao

2017-05-01

Studies of petrology, mineralogy and geochronology of eucrites are keys to reconstruct the thermal and impact history of 4 Vesta, the proposed parent body for HED meteorites. Here we report the petrography, mineralogy and geochemistry of NWA 8009, a newly found eucritic impact-melt breccia, and present SIMS U-Pb ages of zircon and phosphates. NWA 8009 consists of coarse- and fine-grained lithic and mineral clasts set in fine-grained recrystallized matrix. It was derived from a protolith of monomict non-cumulate eucrite. Evidence for intense shock metamorphism observed in NWA 8009 includes mosaicism, deformed exsolution lamellae and partial melting of pyroxene, melting and incipient flow of plagioclase, planar fractures and granular textures of zircon. These shock effects indicate NWA 8009 was subjected to an impact metamorphism with peak pressure of ∼50-60 GPa and post-shock temperature of ∼1160-1200 °C. NWA 8009 is among the most intensely shocked HEDs reported yet. After the impact, the sample was buried near the surface in target rocks and experienced rapid cooling (∼23 °C/h) and annealing, resulting in recrystallization of the matrix and devitrification of plagioclase and silica glasses. U-Pb isotopic system of apatite within plagioclase groundmass of lithic clasts is completely reset and constrains the timing of impact at 4143 ± 61 Ma, providing a new robust impact age on Vesta. Combined with the presence of synchronous impact resetting events, especially those recorded by Lu-Hf, Sm-Nd, and Pb-Pb isotopic systems, we identified a period of high impacts flux at ca. 4.1-4.2 Ga on Vesta. This impact flux occurred coincident with the uptick at ca. 4.1-4.2 Ga in impact age spectra of the moon, probably reflects widespread intense bombardment throughout the inner solar system at ca. 4.1-4.2 Ga. Based on evidence from zircon chemical zoning, petrographic occurrences, as well as the distinctive Zr/Hf ratios, we suggested that zircons in NWA 8009 have had a metamorphic, instead of magmatic origin. They mainly crystallized from melts produced by partial melting of mesostasis area due to reheating event during early global thermal metamorphism, rather than by Zr release from Zr-rich minerals. The U-Pb isotopic system in zircons was not disturbed by subsequent impacts, the weighted-mean 207Pb/206Pb age of 4560 ± 8 Ma represents the timing of zircon growth during thermal metamorphism. Zircons from NWA 8009 and other eucrites may share a common origin during metamorphic growth events, and constraining the global thermal metamorphism on Vesta at ca. 4.55 Ga. The main heat sources responsible for global metamorphism in basaltic crust of Vesta might be heating from the hot interior, especially heat flow related to magmatism, rather than impact.

Ar-Ar Impact Heating Ages of Eucrites and Timing of the LHB

NASA Technical Reports Server (NTRS)

Bogard, Donald; Garrison, Daniel

2009-01-01

Eucrites and howardites, more than most meteorite types, show extensive impact resetting of their Ar-39-Ar-40 (K-Ar) ages approximately equal to 3.4-4.1 Ga ago, and many specimens show some disturbance of other radiometry chronometers as well. Bogard (1995) argued that this age resetting occurred on Vesta and was produced by the same general population of objects that produced many of the lunar impact basins. The exact nature of the lunar late heavy bombardment (LHB or 'cataclysm') remains controversial, but the timing is similar to the reset ages of eucrites. Neither the beginning nor ending time of the lunar LHB is well constrained. Comparison of Ar-Ar ages of brecciated eucrites with data for the lunar LHB can resolve both the origin of these impactors and the time period over which they were delivered to the inner solar system. This abstract reports some new Ar-Ar age data for eucrites, obtained since the authors' 1995 and 2003 papers.

Vesta and the HED Meteorites: Comparison of Spectral Properties

NASA Technical Reports Server (NTRS)

Ammannito, E.; De Sanctis, M. C.; Fonte, S.; Magni, G.; Capaccioni, F.; Tosi, F.; Capria, M. T.; Blewett, D.; Combe, J. P.; Farina, M.;

Movement of Trace Elements During Residence in the Antarctic Ice: a Laboratory Simulation

NASA Technical Reports Server (NTRS)

Strait, Melissa M.

1991-01-01

Recent work has determined that differences in the trace element distribution between Antarctic eucrites and non-Antarctic eucrites may be due to weathering during residence in the ice, and samples that demonstrate trace element disturbances do not necessarily correspond to eucrites that appear badly weathered to the naked eye. This study constitutes a preliminary test of the idea that long-term residence in the ice is the cause of the trace element disturbances observed in the eucrites. Samples of a non-Antarctic eucrite were leached in water at room temperature conditions. Liquid samples were analyzed for rare earth element abundances using ion chromatography. The results for the short-term study showed little or no evidence that leaching had occurred. However, there were tantalizing hints that something may be happening. The residual solid samples are currently being analyzed for the unleached trace metals using instrumental neutron activation analysis and should show evidence of disturbance if the chromatography clues were real. In addition, another set of samples continues to be intermittently sampled for later analysis. The results should give us information about the movement of trace elements under our conditions and allow us to make some tentative extrapolations to what we observe in actual Antarctic eucrite samples.

Composition and Petrology of HED Polymict Breccias: The Regolith of (4) Vesta

NASA Technical Reports Server (NTRS)

Mittlefehldt, David W.; Cartwright, J. A.; Herrin, J. S.; Mertzman, S. A.; Mertzman, K. R.; Peng, Z. X.; Quinn, J. E.

2012-01-01

The polymict breccias of the howardite, eucrite and diogenite (HED) clan of meteorites preserve records of regolith processes that occur on Vesta, their putative home world. These breccias -- howardites, polymict eucrites and polymict diogenites -- are impact-engendered mixtures of diogenites and eucrites. The compositions of polymict breccias can be used to constrain the lithologic diversity of the vestan crust and the excavation depths of these materials. We have done petrological and compositional studies of multiple samples of 5 polymict eucrites and 28 howardites to investigate these issues. Older analyses were done on samples of approx 0.5 gram mass by INAA; newer analyses on samples of approx 5 gram mass by XRF and ICP-MS. We estimate the percentage of eucritic material (POEM) of polymict breccias by comparing their Al and/or Ca contents to those of average basaltic eucrite and diogenite. Our samples have POEM ranging from 28 to 98; adding two polymict diogenites from extends the range to POEM 10. One hypothesis is that ancient, well-mixed vestan regolith has POEM approx 67 and has a higher content of admixed impactor material. Several of our howardites have POEM of 59-74 (Al and/or Ca contents +/- 10% of POEM 67); about a third have Ni contents >300 micro g/g suggesting they contain >2% chondritic material (CM and/or CR). These may be regolithic howardites. Only one (LEW 85313) contains Ne dominated by a solar wind (SW) component. PCA 02066 is dominated by impact-melt material of polymict parentage and petrologically appears to be a mature regolith breccia, yet it does not contain SW-Ne. GRO 95602 falls within the POEM window, contains SW-Ne], yet has a Ni content of 193 micro g/g. Its petrologic characteristics suggest it was formed from immature regolith (no polymict breccia clasts; no glass). Trace element characteristics of the polymict breccias demonstrate the dominance of main-group eucrites as the basaltic component. Mixing diagrams of Zr, Nb, Ba, Hf and Ta with Al show no evidence for a significant contribution from Stannern-trend eucrites. An exception is polymict eucrite LEW 86001 (POEM 92), which is dominated by Stannern-trend basaltic debris. Howardite LAP 04838 (POEM 84) has higher incompatible trace concentrations than other polymict breccias (excluding LEW 86001), and either contains a Stannern-trend basaltic component, or has a significant contributions from evolved eucrites like Nuevo Laredo.

Rocks from Vesta -- Part 1: Eucrites

NASA Image and Video Library

2011-12-02

These images are of HED howardite, eucrite and diogenite meteorites, a large group of meteorites believed to originate from asteroid Vesta, a hypothesis that is consistent with current Dawn observations.

A Howardite-Eucrite-Diogenite (HED) Meteorite Compendium: Summarizing Samples of ASteroid 4 Vesta in Preparation for the Dawn Mission

NASA Technical Reports Server (NTRS)

Garber, J. M.; Righter, K.

2011-01-01

The Howardite-Eucrite-Diogenite (HED) suite of achondritic meteorites, thought to originate from asteroid 4 Vesta, has recently been summarized into a meteorite compendium. This compendium will serve as a guide for researchers interested in further analysis of HEDs, and we expect that interest in these samples will greatly increase with the planned arrival of the Dawn Mission at Vesta in August 2011. The focus of this abstract/poster is to (1) introduce and describe HED samples from both historical falls and Antarctic finds, and (2) provide information on unique HED samples available for study from the Antarctic Meteorite Collection at JSC, including the vesicular eucrite PCA91007, the olivine diogenite EETA79002, and the paired ALH polymict eucrites.

Sm-Nd for Norite 78236 and Eucrite Y980318/433: Implications for Planetary and Solar System Processes

NASA Technical Reports Server (NTRS)

Nyquist, L. E.; Shih, C-Y.; Reese, Y. D.

2008-01-01

Here, we compare Sm-147-Nd-143 and Sm-146-Nd-142 data for lunar norite 78236 to those for approximately 4.54-4.56 Ga old cumulate eucrite Yamato 980318/433 and show that the norite data are compatible with its derivation from an isotopic reservoir similar to that from whence the eucrite pair came. Thus, lunar-like Sm-Nd isotopic systematics are not unique to the Earth-Moon system.

Trace elements record complex histories in diogenites

NASA Astrophysics Data System (ADS)

Balta, J. B.; Beck, A. W.; McSween, H. Y.

2012-12-01

Diogenite meteorites are cumulate rocks composed mostly of orthopyroxene and chemically linked to eucrites (basaltic) and howardites (brecciated mixtures of diogenites and eucrites). Together, they represent the largest single family of achondrite meteorites delivered to Earth, and have been spectrally linked to the asteroid 4 Vesta, the largest remaining basaltic protoplanet. However, this spectral link is non-unique as many basaltic asteroids likely formed and were destroyed in the early solar system. Recent work suggested that Vesta may be an unlikely parent body for the diogenites based on correlations between trace elements and short-lived isotope decay products, which would be unlikely to survive on a body as large as Vesta due to its long cooling history [1]. Recent analyses of terrestrial and martian olivines have demonstrated that trace element spatial distributions can preserve evidence of their crystallization history even when major elements have been homogenized [2]. We have mapped minor elements including Cr, Al, and Ti in seemingly homogeneous diogenite orthopyroxenes and found a variety of previously unobserved textures. The pyroxenes in one sample (GRA 98108) are seemingly large grains of variable shapes and sizes, but the trace elements reveal internal grain boundaries between roughly-equal sized original subgrains, with equilibrated metamorphic triple junctions between them and trace element depletions at the boundaries. These trends suggest extraction of trace elements by a magma along those relict grain boundaries during a reheating event. Two other samples show evidence of fracturing and annealing, with trace element mobility within grains. One sample appears to have remained a closed system during annealing (MET 01084), while the other has interacted with a fluid or magma to move elements along annealed cracks (LEW 88679). These relict features establish that the history of diogenite pyroxenes is more complex than their homogeneous major element compositions imply. Many trace element analyses are performed using either bulk rock techniques or spot analyses, and these maps suggest those types of analyses likely sample variable trace element abundances even within otherwise homogeneous grains, rendering their results difficult to interpret. Consequently, the correlation discussed previously between trace elements and short lived isotopes has likely been impacted by post-magmatic alteration and cannot solely be used to argue that HED's cannot be derived from Vesta. Furthermore, these maps strengthen the HED-Vesta link by suggesting that the diogenites underwent an extended history of cooling, reheating, partial melting, impact fragmentation, fluid/melt migration, and finally re-annealing. These complicated steps are particularly noteworthy as the pyroxene cumulate layer on the asteroid Vesta should lie beneath the eucritic crust, implying that early impacts were able to penetrate that crust and affect the diogenite layers early in Vesta's history, most likely while the asteroid was still hot enough to allow for annealing and regrowth of fractured grains. [1] Schiller et al. (2011) [2] Milman-Barris et al. (2008)

Micrometer-scale U–Pb age domains in eucrite zircons, impact re-setting, and the thermal history of the HED parent body

USGS Publications Warehouse

Hopkins, M.D.; Mojzsis, S.J.; Bottke, W.F.; Abramov, Oleg

2015-01-01

Meteoritic zircons are rare, but some are documented to occur in asteroidal meteorites, including those of the howardite–eucrite–diogenite (HED) achondrite clan (Rubin, A. [1997]. Meteorit. Planet. Sci. 32, 231–247). The HEDs are widely considered to originate from the Asteroid 4 Vesta. Vesta and the other large main belt asteroids record an early bombardment history. To explore this record, we describe sub-micrometer distributions of trace elements (U, Th) and 235,238U–207,206Pb ages from four zircons (>7–40 μm ∅) separated from bulk samples of the brecciated eucrite Millbillillie. Ultra-high resolution (∼100 nm) ion microprobe depth profiles reveal different zircon age domains correlative to mineral chemistry and to possible impact scenarios. Our new U–Pb zircon geochronology shows that Vesta’s crust solidified within a few million years of Solar System formation (4561 ± 13 Ma), in good agreement with previous work (e.g. Carlson, R.W., Lugmair, G.W. [2000]. Timescales of planetesimal formation and differentiation based on extinct and extant radioisotopes. In: Canup, R., Righter, K. (Eds.), Origin of the Earth and Moon. University of Arizona Press, Tucson, pp. 25–44). Younger zircon age domains (ca. 4530 Ma) also record crustal processes, but these are interpreted to be exogenous because they are well after the effective extinction of 26Al (t1/2 = 0.72 Myr). An origin via impact-resetting was evaluated with a suite of analytical impact models. Output shows that if a single impactor was responsible for the ca. 4530 Ma zircon ages, it had to have been ⩾10 km in diameter and at high enough velocity (>5 km s−1) to account for the thermal field required to re-set U–Pb ages. Such an impact would have penetrated at least 10 km into Vesta’s crust. Later events at ca. 4200 Ma are documented in HED apatite 235,238U–207,206Pb ages (Zhou, Q. et al. [2011]. Early basaltic volcanism and Late Heavy Bombardment on Vesta: U–Pb ages of small zircons and phosphates in eucrites. Lunar Planet. Sci. 42. Abstract #2575) and 40–39Ar age spectra (Bogard, D.D. [2011]. Chem. Erde 71, 207–226). Yet younger ages, including those coincident with the Late Heavy Bombardment (LHB; ca. 3900 Ma), are absent from Millbillillie zircon. This is attributable to primordial changes to the velocity distributions of impactors in the asteroid belt, and differences in mineral closure temperatures (Tc zircon ≫ apatite).

Uranium and thorium in achondrites.

NASA Technical Reports Server (NTRS)

Morgan, J. W.; Lovering, J. F.

1973-01-01

The abundances of U and Th in 19 achondrites and two pallasite olivines have been measured by radiochemical neutron activation analysis. Brecciated eucrites are enriched relative to chondrites in both elements by factors between 10 and 20, perhaps as a result of a magmatic differentiation process. Two unbrecciated eucrites are far less enriched, possibly due to their origin as igneous cumulates. The diogenites Johnstown and Shalka contain approximately chondritic levels of U and Th, but Ellemeet is 10 times lower. The abundances in three howardites are in good agreement with those expected from major element data for a mixing model with eucrite and diogenite end members. The high O-18 basaltic achondrites Nakhla, Shergotty and Angra dos Reis have a range of U and Th abundances similar to the brecciated eucrites and howardites, but have systematically higher Th/U ratios.

Lunar and Planetary Science XXXVI, Part 22

NASA Technical Reports Server (NTRS)

2005-01-01

The Lunar and Planetary Science XXXVI, Part 22 is presented. The topics include: 1) Pressure Histories from Thin and Thick Shock-induced Melt Veins in Meteorites; 2) Nano-structured Minerals as Signature of Microbial Activity; 3) The Insoluble Carbonaceous Material of CM Chondrites as Possible Source of Discrete Organics During the Asteroidal Aqueous Phase; 4) Discovery of Abundant Presolar Silicates in Subgroups of Antarctic Micrometeorites; 5) Characteristics of a Seismometer for the LUNAR-A Penetrator; 6) Heating Experiments of the HaH 262 Eucrite and Implication for the Metamorphic History of Highly Metamorphosed Eucrites; 7) Measurements of Ejecta Velocity Distribution by a High-Speed Video Camera; 8) Petrological Comparison of Mongolian Jalanash Ureilite and Twelve Antarctic Ureilites; 9) Metallographic Cooling Rate of IVA Irons Revisited; 10) Inhomogeneous Temperature Distribution in Chondrules in Shock-Wave Heating Model; 11) Subsurface Weathering of Rocks and Soils at Gusev Crater; 12) Extinct Radioactivities in the Early Solar System and the Mean Age of the Galaxy; 13) Correlation of Rock Spectra with Quantitative Morphologic Indices: Evidence for a Single Rock Type at the Mars Pathfinder Landing Site; 14) Silicon Isotopic Ratios of Presolar Grains from Supernovae; 15) Current Status and Readiness on In-Situ Exploration of Asteroid Surface by MINERVA Rover in Hayabusa Mission; 16) Long Formation Period of Single CAI: Combination of O and Mg Isotope Distribution; 17) Supra-Canonical Initial 26Al/27Al Indicate a 105 Year Residence Time for CAIs in the Solar Proto-Planetary Disk; 18) Evolution of Mercury's Obliquity; 19) First Results from the Huygens Surface Science Package; 20) Polyhedral Serpentine Grains in CM Chondrites; 21) Mountainous Units in the Martian Gusev Highland Region: Volcanic, Tectonic, or Impact Related? 22) Petrography of Lunar Meteorite MET 01210, A New Basaltic Regolith Breccia; 23) Earth-Moon Impacts at 300 Ma and 500 Ma Ago; 24) Chemical and Isotopic Analyses of Apollo 16 Glasses: An Integrated Approach; 25) Measuring the Surfaces on Mars; 26) Melting in Martian Snowbanks; 27) The Effect of Ni on Fe-FeS Phase Relations: Implications for the Chemistry of the Martian Core; 28) Shorelines in the Western United States as Analogs for Hypothesized Shoreline Features on Mars; 29) Al and Ti Isotopic Ratios of Presolar SiC Grains of Type Z; 30) Physicochemical Conditions of Clinopyroxene Crystallization in the Parental Bodies of Ordinary Chondrites; 31) Metamorphosed CM and CI Carbonaceous Chondrites Could be from the Breakup of the Same Earth-crossing Asteroid; 32) Aqueous Alteration and Hydrogen Generation on Parent Bodies of Unequilibrated Ordinary Chondrites: Thermodynamic Modeling for the Semarkona Composition; and 33) Preliminary Analysis of Relative Abundances of Hydrothermal Alteration Products in the C1-N10, Y6-N19, and Yax-1_863.51 Impact Melt Samples, Chicxulub Structure, Mexico

Petrology and Geochemistry of the NWA 3368 Eucrite

NASA Astrophysics Data System (ADS)

Gardner, K. G.; Lauretta, D. S.; Hill, D. H.; Goreva, J. S.; Domanik, K. J.; Franchi, I. A.; Drake, M. J.

2006-03-01

We report the petrology and geochemistry of NWA 3368, a new non-cumulate, monomict eucrite breccia with a variety of clast sizes and a pink-tinted matrix. Analytical techniques include electron microprobe, INAA, and ICP-MS.

Northwest Africa 1109 and Camel Donga: Metal-bearing Brecciated Eucrites

NASA Astrophysics Data System (ADS)

Isa, J.; Yamaguchi, A.; Shinotsuka, K.; Ebihara, M.

2009-03-01

Two eucrites NWA1109 and Camel Donga contain significant amounts of Fe-metals. In order to better understand the origin of the Fe-metals, we performed a petrological and geochemical study of these meteorites.

Compositional Diversity of the Vestan Regolith Derived from Howardite Compositions and Dawn VIR Spectra

NASA Technical Reports Server (NTRS)

Mittlefehldt, D. W.; Ammannito, E.; Hiroi, T.; DeAngeles, S.; Moriarty, D. P.; DiIorio, T.; Pieters, C. M.; DeSanctis, M. C.

2014-01-01

Howardite, eucrite and diogenite meteorites likely come from asteroid 4 Vesta [1]. Howardites - physical mixtures of eucrites and diogenites - are of two subtypes: regolithic howardites were gardened in the true regolith; fragmental howardites are simple polymict breccias [2]. The Dawn spacecraft imaged the howarditic surface of Vesta with the visible and infrared mapping spectrometer (VIR) resulting in qualitative maps of the distributions of distinct diogenite-rich and eucrite-rich terranes [3, 4]. We are developing a robust basis for quantitative mapping of the distribution of lithologic types using spectra acquired on splits of well-characterized howardites [5, 6]. Spectra were measured on sample powders sieved to <75 µm in the laboratories of the Istituto di Astrofisica e Planetologia Spaziali and Brown University. Data reduction was done using the methods developed to process Dawn VIR spectra [4]. The band parameters for the 1 and 2 µm pyroxene absorption features (hereafter BI and BII) can be directly compared to Dawn VIR results. Regolithic howardites have shallower BI and BII absorptions compared to fragmental howardites with similar compositions. However, there are statistically significant correlations between Al or Ca contents and BI or BII center wavelengths regardless of howardite subtype. Diogenites are poor in Al and Ca while eucrites are rich in these elements. The laboratory spectra can thus be directly correlated with the percentage of eucrite material contained in the howardites. We are using these correlations to quantitatively map Al and Ca distributions, and thus the percentage of eucritic material, in the current regolith of Vesta.

An Amoeboid Olivine Aggregate in LEW 85300

NASA Technical Reports Server (NTRS)

Komatsu, M. D.; Yamaguchi, A.; Fagan, T. J.; Zolensky, M. E.; Shiran, N.; Mikouchi, T.

2016-01-01

Amoeboid Olivine aggregates (AOAs) are irregularly shaped objects commonly observed in carbonaceous chondrites. Because they are composed of fine-grained olivine and Ca-Al-rich minerals, they are sensitive indicators for nebular process and parent body alteration of their parent bodies. Recently an AOA was found in a carbonaceous clast in polymict eucrite LEW 85300. The bulk major element composition of the clast matrix in LEW 85300 suggests a relation to CM, CO and CV chondrites, whereas bulk clast trace and major element compositions do not match any carbonaceous chondrite, suggesting they have a unique origin. Here we characterize the mineralogy of AOA in LEW 85300 and discuss the origin of the carbonaceous clasts. Results and Discussion: The AOA is located in an impact melt vein. Half of the aggregate shows recrystallization textures (euhedral pyroxene and molten metal/FeS) due to impact melting, but the remaining part preserves the original texture. The AOA is composed of olivine, FeS and Mg,Al-phyllosilicate. Individual olivine grains measure 1-8 microns, with Fe-rich rims, probably due to impact heating. Olivines in the AOA are highly forsteritic (Fo95-99), indicating that the AOA escaped thermal metamorphism [4]. Although no LIME (Low-Fe, Mn-Enriched) olivine is observed, forsterite composition and the coexistence of Mg,Al-phyllosilicate suggest that the AOA is similar to those in the Bali-type oxidized CV (CVoxB) and CR chondrites. However, it should be noted that fayalitic olivine, which commonly occurs in CVoxB AOA, is not observed in this AOA. Also, the smaller grain size (<8 microns) of olivine suggests they may be related to CM or CO chondrites. Therefore, we cannot exclude the possibility that the AOA originated from a unique carbonaceous chondrite.

Laboratory spectroscopy of HED meteorites

NASA Astrophysics Data System (ADS)

Farina, M.; Coradini, A.; Carli, C.; Ammannito, E.; Consolmagno, G.; De sanctis, M.; Di Iorio, T.; Turrini, D.

2011-12-01

4 Vesta is one of the largest and the most massive asteroid in the Main Asteroid Belt. This asteroid possesses a basaltic surface and apparently formed and differentiated very early in the history of the solar system. There are strong evidences that indicate Vesta as the parent body of Howardites, Diogenites and Eucrites (HEDs). HED meteorites are a subgroup of achondrite meteorites and they are a suite of rocks that formed at high temperature and experienced igneous processing similar to the magmatic rocks found on Earth. The visible and near-infrared (VNIR) reflectance spectra of Vesta's surface show high similarity with the laboratory spectra of HED meteorites. Vesta and HEDs spectra have two crystal field absorption bands close to 0.9 μm and 1.9 μm indicative of the presence of ferrous iron in pyroxenes. The HEDs differ from each other primarily based on variation in pyroxene composition and the pyroxene-plagioclase ratio as well as rocks texture characteristics (e.g., size of crystals). These differences suggest that a combined VNIR spectra studies of Vesta and HED meteorites might reveal the different characteristics of the surface compositions and shed new light on the origin and the thermal history of Vesta. Moreover the link between Vesta and HEDs could provide a test bed to understand the short-lived radionuclide-driven differentiation of planetary bodies. Here we present preliminary result of a study of spectral characteristics of different HED samples, provided to us by the Vatican Observatory. Bidirectional reflectance spectra of slabs of meteorites are performed in the VNIR, between (0.35/2.50) μm, using a Fieldspec spectrometer mounted on a goniometer, in use at the SLAB (Spectroscopy laboratory, INAF, Rome). The spectra are acquired in standard conditions with an incidence angle i=30o and an emission angle e=0o, measuring a spot with a diameter of 5 mm. Different Howardite, Diogenite and Eucrite samples are "mapped" considering several spots on the surface of the slabs to define their spectral variability between samples representing the different types of HEDs and to describe the spectral heterogeneity for each samples. A preliminary comparison with mineralogical and petrographic characteristics has been done describing hand samples and their thin sections. These data will be incorporated in a spectral library that could be an useful tool for the interpretation of data acquired by the Dawn mission in orbit on Vesta.

Revisiting NWA 3141, 8266 and 8594; Two Eucrites and a Howardite?

NASA Astrophysics Data System (ADS)

Mitchell, J. T.; Stephen, N. R.

2016-08-01

SEM analysis was used to study the petrology of monomict eucrites Northwest Africa 3141, 8594 and 8266. The analysis carried out in this study supports the official classifications of NWA 3141 and 8594, but suggests NWA 8266 is a polymict breccia.

Vesta's Elemental Composition

NASA Technical Reports Server (NTRS)

Prettyman, T. H.; Beck, A. W.; Feldman, W. C.; Lawrence, D. J.; McCoy, T. J.; McSween, H. Y.; Mittlefehldt, D. W.; Peplowski, P. N.; Raymond, C. A.; Reedy, R. C.;

Origin of igneous meteorites and differentiated asteroids

NASA Astrophysics Data System (ADS)

Scott, E.; Goldstein, J.; Asphaug, E.; Bottke, W.; Moskovitz, N.; Keil, K.

2014-07-01

Introduction: Igneously formed meteorites and asteroids provide major challenges to our understanding of the formation and evolution of the asteroid belt. The numbers and types of differentiated meteorites and non-chondritic asteroids appear to be incompatible with an origin by fragmentation of numerous Vesta-like bodies by hypervelocity impacts in the asteroid belt over 4 Gyr. We lack asteroids and achondrites from the olivine-rich mantles of the parent bodies of the 12 groups of iron meteorites and the ˜70 ungrouped irons, the 2 groups of pallasites and the 4--6 ungrouped pallasites. We lack mantle and core samples from the parent asteroids of the basaltic achondrites that do not come from Vesta, viz., angrites and the ungrouped eucrites like NWA 011 and Ibitira. How could core samples have been extracted from numerous differentiated bodies when Vesta's basaltic crust was preserved? Where is the missing Psyche family of differentiated asteroids including the complementary mantle and crustal asteroids [1]? Why are meteorites derived from far more differentiated parent bodies than chondritic parent bodies even though C and S class chondritic asteroids dominate the asteroid belt? New paradigm. Our studies of meteorites, impact modeling, and dynamical studies suggest a new paradigm in which differentiated asteroids accreted at 1--2 au less than 2 Myr after CAI formation [2]. They were rapidly melted by 26Al and disrupted by hit-and-run impacts [3] while still molten or semi-molten when planetary embryos were accreting. Metallic Fe-Ni bodies derived from core material cooled rapidly with little or no silicate insulation less than 4 Myr after CAI formation [4]. Fragments of differentiated planetesimals were subsequently tossed into the asteroid belt. Meteorite evidence for early disruption of differentiated asteroids. If iron meteorites were samples of Fe-Ni cores of bodies that cooled slowly inside silicate mantles over ˜50--100 Myr, irons from each core would have almost indistinguishable cooling rates as thermal gradients across cores would have been minimal. Irons in groups IIIAB, IVA, and IVB have chemical crystallization trends showing that they cooled in three separate bodies. However, each shows a wide range of cooling rates [4]. Group IVA irons cooled through 500°C at 6600--100 °C/Myr in a metallic body of radius 150 ± 50 km with scarcely any silicate insulation [5]. The Pb-Pb age of 4565.3 ± 0.1 Myr for a IVA iron [6] confirms that these irons cooled to ˜300°C only 2--3 Myr after CAI formation. Multiple hit-and-run impacts may have separated core and mantle material during accretion [7] as hypervelocity impacts do not efficiently separate cores from mantles. Thermal histories and magnetic properties of main group pallasites also require early catastrophic disruption of their primary parent body [8,9]. Conclusions. The anomalous properties of differentiated asteroids and meteorites cannot be explained by concealing differentiated planetesimals under chondritic crusts [10] as meteorite breccias and the apparent compositional homogeneity of asteroid families are inconsistent with this model. Like Burbine et al. [11], we attribute the lack of olivine mantle meteorites and asteroids to collisional grinding of weaker silicate and the preferential survival of stronger metallic Fe,Ni fragments. But we infer that asteroid break up occurred very early inside 2 au, not in the asteroid belt over 4 Gyr. Vesta may have preserved its crust due to early ejection into the asteroid belt. It is the smallest terrestrial planet --- not an archetypal differentiated asteroid.

The Abundance and Isotopic Composition of Water in Howardite-Eucrite-Diogenite Meteorites

NASA Astrophysics Data System (ADS)

Barrett, T. J.; Tartèse, R.; Anand, M.; Franchi, I. A.; Grady, M. M.; Greenwood, R. C.; Charlier, B. L. A.

2014-09-01

Using SIMs techniques we measure OH abundances and D/H ratios in apatite grains from two Eucrites (DaG 945, DaG 844).The average δD values of these two samples are also similar to carbonaceous chondrites, the Earth and the Moon.

The Regolith of 4 Vesta: Perspectives from Howardite Meteorites and Dawn Mission Observations

NASA Technical Reports Server (NTRS)

Mittlefehldt, David W.; Blewett, David T.; Denevi, Brett W.; DeSanctis, M. C.; Jaumann, Ralf; Keller, H. Uwe; Nathues, Andreas; Pieters, Carle M.; Raymond, C. A.; Zuber, Maria T.

2011-01-01

4 Vesta is the largest asteroid with a basaltic surface, the only surviving differentiated asteroid recording igneous processes from the earliest phase of solar system history. The Dawn spacecraft is in orbit about Vesta pursuing a campaign of high resolution imaging and visible and infrared spectrometry of the surface; compositional mapping by gamma-ray and neutron spectrometry will follow. Vesta is heavily cratered with a surface covered by impact debris, a regolith. One important goal of the Dawn mission is to develop an understanding of regolith processes that are affecting this surface debris. Regolith characteristics are a record of interaction with the environment (e.g., impactors, dust, solar wind, galactic cosmic-rays) and give evidence of surface processes (down-gravity movement, etc.). Regolith mineralogy and composition reflect the local bedrock, with influences from regional and global mixing. Understanding regolith processes will aid in determining the lithology of underlying crust. Vesta is most likely the parent asteroid of the howardite, eucrite and diogenite meteorites. Eucrites are intrusive and extrusive mafic rocks composed mostly of ferroan low-Ca clinopyroxene and calcic plagioclase, while diogenites are cumulate magnesian orthopyroxenites. Magmatism occurred within a few million years of the formation of the solar system and then ceased. Impacts into the igneous crust produced the howardites - polymict breccias composed of mineral and lithic debris derived mostly from eucrites and diogenites. Some howardites are true regolith breccias formed by lithification of extensively impact-gardened surface debris. However, howardites have a number of significant petrologic and compositional differences from mature lunar regolith breccias and soils reflecting the different environment around Vesta compared to that at 1 AU. The most significant differences are the higher impactor flux with a lower mean impact velocity and the lower gravity. As a result, regolith processes on Vesta differ in detail from those on the Moon. Laboratory study of howardites and orbital investigation of Vesta will allow for development of robust models of regolith formation on hand sample to multi-kilometer scales.

A Cabonaceous Chondrite Dominated Lithology from the HED Parent; PRA 04401

NASA Technical Reports Server (NTRS)

Herrin, Jason S.; Zolensky, M. E.; Mittlefehldt, David W.

2010-01-01

The paired howardite breccias Mt. Pratt (PRA) 04401 and PRA 04402 are notable for their high proportion of carbonaceous chondrite clasts [1]. They consist predominantly of coarse (0.1-7 mm) diogenite (orthopyroxene), eucrite (plagioclase + pyroxene), and carbonaceous chondrite clasts set in a finer grained matrix of these same materials. Coarse C-chondrite clasts up to 7 mm are composed mainly of fine-grained phyllosilicates with lesser sulfides and high-mg# anhydrous magnesian silicates. Most of these clasts appear to be texturally consistent with CM2 classification [1] and some contain relict chondrules. The clasts are angular and reaction or alteration textures are not apparent in the surrounding matrix. PRA 04401 contains about 70 modal% C-chondrite clasts while PRA 04402 contains about 7%. Although many howardites are known to contain abundant C-chondrite clasts [2,3,4], PRA 04401 is, to our knowledge, the most chondrite-rich howardite lithology identified to date. Low EPMA totals from CM2-type clasts in other howardites suggest that they frequently contain 10 wt% or more water [2], a figure consistent with their mineralogy. PRA 04401, therefore, demonstrates the potential for hydrous lithologies with greater than 5 wt% water to occur locally within the nominally anhydrous HED parent body. Since the origin of this water is xenogenic, it might therefore be concentrated in portions of the asteroid surface where it would be more readily observable by remote sensing techniques. We plan to further examine C-chondrite clasts in PRA 04401/2 with the intent of establishing firm chemical classification, estimating water content, and evaluating their relationship with the host breccia. To help place them in context of the HED parent, we will also compare these breccias with other howardites to evaluate which lithologies are likely to be more prevalent on the asteroid surface.

Redox History of Early Solar System Planetismals Recorded in the D;Orbigny Angrite

DOE Office of Scientific and Technical Information (OSTI.GOV)

King, P.L.; Sutton, S.R.; Spilde, M.N.

2012-04-02

Angrites are ancient basaltic meteorites ({approx}4.56 Ga) that preserve evidence of some of the solar system's earliest melting events. The volcanic-textured angrites such as D'Orbigny were rapidly crystallized and are relatively pristine; lacking shock, brecciation, and parent-body weathering textures. Thus, these angrites provide a unique 'window' into the petrogenesis of planetary bodies in the early solar system. Angrites may be formed by partial melting of CV chondrites under relatively oxidized sources compared to the eucrites, and therefore may document variations in fO{sub 2} conditions on carbonaceous chondrite parent bodies. Thus, understanding the intrinsic fO{sub 2} conditions of the angrites ismore » needed to determine how different early Solar System basalts form, to model separation of the core, mantle and crust, and to understand magnetic fields on planetary bodies. The D'Orbigny angrite contains a range of textures: (a) crystalline texture containing interlocking crystals of fassaite (pyroxene) with Ti-rich rims, anorthite, and Mg-olivine with Fe-rich rims; (b) cavities with protruding needle-like pyroxene and anorthite dusted by Ca-(Mg)-carbonate; (c) mesostasis with kirschsteinite, ilmenite, troilite, phosphates (e.g., merrilite, whitlockite and Casilicophosphate), rhonite and minor glass; (d) glasses ({approx} angrite composition) in vesicles, as inclusions and as beads, and also cross-cutting crystal-rich portions of the rock; (e) vesicles (e.g., {approx}1.4 vol. %, 0.0219-87.7 mm{sup 3}). Analysis of the textures and Fe{sup 3+}/Fetotal of the cavity pyroxene suggests that the oxygen fugacity (fO{sub 2}) increased in the D'Orbigny angrite perhaps due to introduction of a gas phase. Here we examine the detailed fO{sub 2} history using micro-analyses that allow us to avoid inclusions that may cause spurious results. We present analyses of both S- and V- oxidation states to complement other work using Fe-oxidation state and to avoid problems related to measuring low concentrations of Fe{sup 3+} and propagating errors when calculating fO{sub 2} in samples with low Fe{sup 3+} concentrations.« less

Partial melting of the Allende (CV3) meteorite - Implications for origins of basaltic meteorites

NASA Technical Reports Server (NTRS)

Jurewicz, A. J. G.; Mittlefehldt, D. W.; Jones, J. H.

1991-01-01

Eucrites and angrites are distinct types of basaltic meteorites whose origins are poorly known. Experiments in which samples of the Allende (CV3) carbonaceous chondrite were partially melted indicate that partial melts can resemble either eucrites or angrites, depending only on the oxygen fugacity. Melts are eucritic if this variable is below that of the iron-wuestite buffer or angritic if above it. With changing pressure, the graphite-oxygen redox reaction can produce oxygen fugacities that are above or below those of the iron-wuestite buffer. Therefore, a single, homogeneous, carbonaceous planetoid greater than 110 kilometers in radius could produce melts of drastically different composition, depending on the depth of melting.

Valence State Partitioning of Cr and V Between Olivine-Melt and Pyroxene-Melt in Experimental Basalts of a Eucritic Composition

NASA Technical Reports Server (NTRS)

Karner, J. M.; Jones, J. H.; Le, L.

2017-01-01

The partitioning of multivalent elements in basaltic systems can elucidate the oxygen fugacity (fO2) conditions under which basalts formed on planetary bodies (Earth, Moon, Mars, asteroids). Chromium and V are minor and trace elements in basaltic melts, partition into several minerals that crystallize from basaltic melts, exist in multiple valence states at differing fO2 conditions, and can therefore be used as oxybarometers for basaltic melts. Chromium is mostly 3+ in terrestrial basaltic melts at relatively high fO2 values (= IW+3.5), and mostly 2+ in melts at low fO2 values (= IW-1), such as those on the Moon and some asteroids. At intermediate fO2s, (i.e., IW-1 to IW+3.5), basaltic melts contain both Cr3+ and Cr2+. Vanadium in basaltic melts is mostly 4+ at high fO2, mostly 3+ at low fO2, and a mix of V3+ and V4+ at intermediate fO2 con-ditions. Understanding the partitioning of Cr and V into silicate phases with changing fO2 is therefore critical to the employment of Cr and V oxybarometers. In this abstract we examine the equilibrium partitioning of Cr and V between olivine/melt and pyroxene/melt in experimental charges of a eucritic composition produced at differing fO2 conditions. This study will add to the experimental data on DCr and DV (i.e., olivine/melt, pyroxene/melt) at differing fO2, and in turn these D values will be used to assess the fO2 of eucrite basalts and perhaps other compositionally similar planetary basalts.

Alteration of Labile Trace Element Concentrations in Antarctic Meteorites by Weathering: A Five-Year Assessment

NASA Astrophysics Data System (ADS)

Wang, M.-S.; Xiao, X.; Lipschutz, M. E.

1992-07-01

Numerous studies since 1987 demonstrate that, on average, Antarctic populations of specific meteorite groups differ from non-Antarctic falls. Some differences could conceivably reflect alteration during the meteorites' residence in Antarctica while others clearly are preterrestrial origin, predating fall on Earth. Concentrations of certain trace elements (Ag, Au, Bi, Cd, Co, Cs, Ga, In, Rb, Sb, Se, Te, Tl, Zn) determined by RNAA in 45 H4-6 chondrites first provided evidence for Antarctic/non-Antarctic meteorite population differences [1]. Most of these elements are thermally labile (easily lost during extended chondritic heating chondrites) so that their concentrations give important information on the thermal history of meteoritic material. Refractory elements cannot give such information. Factors possibly complicating establishment of compositional differences as preterrestrial--meteorite pairing, population reproducibility, analyst bias, and statistical modeling--are of demonstrated in consequence [1-4]. Indeed, compositional differences exist [3,4] between Antarctic meteorite populations (Victoria Land vs. Queen Maud Land) and among observed falls (Cluster 1 vs. other falls). Possibilities for meteorite compositional alteration during Antarctic weathering must be re-assessed as new data are obtained: here, we summarize the current status of this problem. 1. Highly weathered meteorites: Ten of our suite of trace elements have significantly lower mean concentrations (presumably because of leaching) in H5 chondrites of weathering types B/C and C, than in types A, A/B, and B [1]. Meteorites of types A to B-- whether exhibiting efflorescence or not--seem uncompromised [5]. 2. Antarctic meteorites of high weathering susceptibility: Carbonaceous chondrites and lunar meteorites are essentially unaltered by weathering. For example, data for LEW 90500 C(1?) chondrite reported here demonstrate that the 8 most volatile elements (Se, Cs, Te, Zn, Cd, Bi, Tl, In) have a mean Cl- normalized weight ratio of 0.585+-0.069. Other elements--even Rb, which should be easily transported in a phyllosilicate exposed to water--show no evidence for gain or loss in Antarctica. This is true also for 39 other Antarctic C2-6 chondrites [6]; 3 additional Cl-2 chondrites thermally metamorphosed in their parent bodies [7]; and lunar meteorites studied by us and others. Hydration effects are absent in these meteorites. 3. Eucrites exhibiting evidence for Ce transport: A pair of eucrite clast samples (EET 87503,23 interior and exterior), was previously studied by INAA yield REE data suggesting addition of LREE (except Ce) to the interior during Antarctic residence (Mittlefehldt, personal communication). The exterior/interior ratio for Ce, 1.1, is the same as the mean value for our RNAA trace element suite, 1.1+-0.5. Despite the large uncertainty of this ratio (reflecting the normally heterogeneous distribution of labile elements in eucrites--including falls [8]), results for EET 87503,23 are consistent with the interpretation that our suite of labile trace elements is unaffected by the process that affected REE other than Ce. Our elements are probably dispersed among many host sites, rather than being sited in a single host, like whitlockite. More RNAA measurements of additional eucrite pairs should be done to confirm this result. Further, a putative C3 clast exhibits no evidence for terrestrial alteration of RNAA elements, saponitic matrix, etc. even though REE have apparently been leached from basalts in its host eucrite, LEW 85300 [5]. After five years, numerous investigations confirm meteorite population differences consistent with the RNAA results. While Antarctic processes may have affected REE contents in some eucrites, at present no evidence exists for labile trace element transport into/out of interiors of meteorites of weathering types A to B. The absence of evidence is not evidence of absence, so continued vigilance remains necessary. Research supported by NASA grant NAG 9-48, aided by DOE grant DE-FG07-80ER10725J and NATO grant 0252/89. References: 1. Dennison J. E. and Lipschutz M. E. (1987) Geochim. Cosmochim. Acta 51, 741-754. 2. Lipschutz M. E. and Samuels S. M. (1991) Geochim. Cosmochim. Acta 55, 19-34. 3. Wolf S. F. and Lipschutz M. E. (1992) Lunar Planet. Sci. (abstract) XXIII, 1545-1546. 4. Wolf S. F. and Lipschutz M. E. (abstract), this conference. 5. Zolensky M. E., Hewins R. H., Mittlefehldt D. W., Lindstrom M. M., Xiao X., and Lipschutz M. E. (1992) Meteoritics, submitted. 6. Xiao X. and Lipschutz M. E. (1992) J. Geophys. Res. Planets, in press. 7. Paul R. L. and Lipschutz M. E. (1989) Z. Naturf. 44a, 978-987. 8. Paul R. L. and Lipschutz M. E. (1990) Geochim. Cosmochim. Acta 54, 3185-3195.

The Pasamonte unequilibrated eucrite: Pyroxene REE systematic and major-, minor-, and trace-element zoning. [Abstract only

NASA Technical Reports Server (NTRS)

Pun, A.; Papike, J. J.

1994-01-01

We are evaluating the trace-element concentrations in the pyroxenes of Pasamonte. Pasamonte is a characteristic member of the main group eucrites, and has recently been redescribed as a polymict eucrite. Our Pasamonte sample contained eucritic clasts with textures ranging from subophitic to moderately coarse-grained. This study concentrates on pyroxenes from an unequilibrated, coarse-grained eucrite clast. Major-, minor-, and trace-element analyses were measured for zoned pyroxenes in the eucritic clast of Pasamonte. The major- and minor-element zoning traverses were measured using the JEOL 733 electron probe with an Oxford-Link imaging/analysis system. Complemenatry trace elements were then measured for the core and rim of each of the grains by SIMS. The trace elements analyzed consisted of eight REE, Sr, Y, and Zr. These analyses were performed on a Cameca 4f ion probe. The results of the CI chondrite normalized (average CI trace-element analyses for several grains and the major- and minor-element zoning patterns from a single pyroxene grain are given. The Eu abundance in the cores of the pyroxenes represents the detection limit and therefore the (-Eu) anomaly is a minimum. Major- and minor-element patterns are typical for igneous zoning. Pyroxene cores are Mg enriched, whereas the rims are enriched in Fe and Ca. Also, Ti and Mn are found to increase, while Cr and Al generally decrease in core-to-rim traverses. The cores of the pyroxenes are more depleted in the Rare Earth Elements (REE) than the rims. Using the minor- and trace-element concentrations of bulk Pasamonte and the minor- and trace-element concentrations from the cores of the pyroxenes in Pasamonte measured in this study, we calculated partition coefficients between pyroxene and melt. This calculation assumes that bulk Pasamonte is representative of a melt composition.

Northwest Africa 5738: Multistage fluid-driven secondary alteration in an extraordinarily evolved eucrite

NASA Astrophysics Data System (ADS)

Warren, Paul H.; Rubin, Alan E.; Isa, Junko; Gessler, Nicholas; Ahn, Insu; Choi, Byeon-Gak

2014-09-01

The Northwest Africa 5738 eucrite contains a record of unprecedented geochemical complexity for a sample from the HED asteroid. It originated with a uniquely evolved (Stannern Trend) primary igneous composition, combining ultra-high bulk incompatible element and Na2O concentrations with a relatively low mg. Its bulk oxygen-isotopic composition (Δ‧17O = -0.27‰), as well as its trace element composition (e.g., Ga/Al), confirm other evidence for classification as a eucrite. Pyroxene mg equilibration, exsolution and ;cloudy; inclusions, all reflect a typical eucritic degree of thermal metamorphism. The rock contains an unprecedented array of microscopic fluid-metasomatic vein deposits. Most common are curvy microveins within pyroxene, which consist dominantly of Ca-plagioclase (typically An95, in stark contrast with the rock's An68-78 primary-igneous plagioclase), with Fe-olivine (Fo14) and Cr-spinel as additional major constituents. Likely related to these microveins are small masses of intergrown Ca-plagioclase (again roughly An95) and silica (or high-Si glass). Analyses of the microvein Cr-spinels show stoichiometry implying a significant Fe3+ content (Fe2O3 0.7-2.3 wt.%), and fO2 up to roughly IW+3; clearly elevated in comparison to the normal HED fO2 of about IW-1. The fO2 results show an anticorrelation with equilibration T (and with Mg/Fe), which suggests the parent fluid system became more oxidizing as it cooled. NWA 5738 also contains apparent secondary iron metal. The Fe-metals are very pure, with Ni consistently below an EPMA detection limit of ∼0.01 wt.%. The vein-like shapes of roughly 1/3 of the largest Fe-metals suggest origin by deposition from a fluid. The role of pyroxene exsolution as template for a denticular (sawtooth) Fe-metal edge shape, and the survival of Fo14 olivine in a rock with abundant silica and a far higher bulk mg, suggest that the most intense thermal metamorphism occurred no later than the secondary alteration. Near-complete lack of spatial association suggests that the Fe-metals formed during a distinct time period from the curvy microveins. The immediate cause of Fe-metal deposition was most plausibly (or anyway, least implausibly) an abrupt downshift in the fluid fO2. Considering the extremely evolved bulk composition, the fluid(s) may have been largely deuteric. However, more likely the main source of fluid was a nearby buried mass of volatile-rich impactor matter, such as carbonaceous chondrite, that hit the asteroid at low enough velocity to remain mostly intact. We further speculate that the abrupt drop in fluid fO2 may have been caused by a process of carbon-fueled ;smelting; (cf. ureilites), triggered by an impact-effected shift of the carbonaceous material to a changed environment, with higher T and/or lower P. These and other recent eucrite results point to a need for greater scrutiny regarding the absence of comparable alteration-veining in rocks from the lunar highland crust, a mysterious lack in view of recent evidence for abundant lunar water.

Glass Veins in the Unequilibrated Eucrite Yamato 82202

NASA Technical Reports Server (NTRS)

Bogard, Donald; Buchanan, Paul; Noguchi, T.; Katavama, Ikuo

2004-01-01

The unequilibrated eucrite Yamato 82202 (Y82202) contains a network of glass veins, which are relatively thick (up to 1 mm in width) and are not devitrified. The host of the meteorite represents volcanic rock that crystallized >4.3 Gyr ago, probably as a lava flow on the surface of 4 Vesta. The impact event that formed the glass veins occurred at approx. 3.9 Gyr under conditions of low effective fo2 and very rapid cooling. A S-rich vapor probably was generated by impact vaporization of sulfides. The impact melt was not superheated and it retains some disordered structural characteristics of the original pyroxene and feldspar of the eucritic target lithology. The unequilibrated pyroxenes of this eucrite and the pristine character of the glass indicate that the meteorite experienced no significant metamorphism after initial crystallization. Hence, it was not buried to a significant depth or covered by a lava flow or hot layer of impact ejecta. The meteorite resided at a shallow level (though not at the surface) on 4 Vesta or on one of the vestoids until it was ejected and traveled to Earth, probably with other HED materials that have Ar-36 exposure ages of approx. 13 Myr.

Lu-Hf systematics of meteorites

NASA Astrophysics Data System (ADS)

Bizzarro, M.; Baker, J. A.; Haack, H.

2003-04-01

We have measured Lu-Hf concentrations and Hf isotope ratios on a number of solar system objects with a new digestion and chemical separation technique (1). The analysed materials include a variety of carbonaceous and ordinary chondrites (CC and OC), basaltic eucrites and a diogenite, and work is ongoing on angrites, aubrites and mesosiderites. Nineteen analyses of OC and CC define, for the first time, a statistically significant Lu-Hf isochron with a slope of 0.09465 ± 145 and intercept of 0.279628 ± 47 (2). In contrast to the CC and type 3 OC (176Lu/177Hf = 0.032-0.034), the more highly metamorphosed OC have a large range of 176Lu/177Hf ratios (0.026-0.036). The large range of 176Lu/177Hf values may be related to heterogeneous variations in phosphate abundances in equilibrated OC, which is supported by the observation that most of the observed variation is defined by this type of material. The present-day bulk-earth 176Hf/177Hf ratio calculated from this study, and a 176Lu/177Hf ratio of 0.0332, is identical to the value of (3) and confirms that the chondritic Hf-Hd isotopic composition is displaced (3 ɛ units) to unradiogenic Hf compared to the terrestrial array. The slope and intercept derived from individual regressions of either the OC or the L type alone are identical within analytical uncertainty. Using a mean age of 4.56 Ga for the chondrite forming event, we derive a value for λ176Lu = 1.983 ± 33 time 10-11 y-1 from the regression of the chondrite meteorites, ca. 6% faster than a recent calibration based on terrestrial material, which has important implications for the differentiation of the early Earth (2, 4). The four basaltic eucrites analysed align on the same array as the chondrites and, as such, chondrites and basaltic eucrites also define a statistically significant isochron with a slope of 0.09462 ± 68 and intercept of 0.279627 ± 20, identical to the values derived from the chondrites alone. Moreover, a recent Lu-Hf study of basaltic eucrites also yielded a slope and intercept identical to that determined here (5). In contrast, three cumulate eucrites of (5) and our analysis of the Bilanga diogenite align on a statistically significant Lu-Hf isochron defining an age of 4.349 ± 0.073 Ga. This implies a genetic relationship between diogenites and cumulate eucrites, and further confirms that cumulate eucrites are at least 100 Myr younger than basaltic eucrites. (1) Bizzarro, M., Baker, J.A. &Ulfbeck D. (in review) Geostandards Newsletter. (2) Bizzarro, M., Baker, J.A., Haack, H., Ulfbeck D. &Rosing M. (In press) Nature. (3) Blichert-Toft, J. &Albarede, F. (1997) EPSL 148, 243-258. (4) Scherer, E., Münker, C. &Mezger, K. (2001) Science 293, 683-686. (5) Blichert-Toft, J., Boyet, M., Télouk, P &Albarède, F. (2002) EPSL 204, 167-181.

Diogenites: Cumulates from Asteroid 4 Vesta: Insights from Orthopyroxene and Spinel Chemistry

NASA Technical Reports Server (NTRS)

Papike, James J.; Bowman, L. E.; Spilde, M. N.; Fowler, G. W.; Shearer, C. K.

1996-01-01

Cumulate rocks are important planetary lithologies, but they can be difficult to interpret. Important clues to the nature of their parental melts may still be present in the interiors of cumulus phases. However, in some cases, even the cores of the cumulus grains may have been modified by postcrystallization reactions with trapped melt and other cumulus phases. We have previously studied the major-, minor-, and trace-element chemistry of orthopyroxene from a suite of diogenites and concluded that their chemical attributes can best be explained by crystallization from parental melts that were derived from a depleted mantle source that had already experienced eucrite removal. However, we and others have had difficulty explaining the great range in concentration of minor elements (Al, Ti) and trace elements (REE, Y, Zr) if all diogenites were derived from a single magmatic system. Therefore, we have investigated the chemistry of diogenitic spinels to see if they still held clues to the diogenite parental melt compositions. Although spinel is low in abundance in diogenites (<5 vol%) it still may hold clues to the maomatic and metamorphic history of these rocks.

On the origin of the moon, with emphasis on bulk composition

NASA Technical Reports Server (NTRS)

Kaula, W. M.

1977-01-01

A new analysis of altimetric, gravimetric, and seismological results, together with petrological and thermal history constraints, obtains an estimated Al2O3 content of 5.0%, 2.1 times chondritic. Hence the moon definitely has a refractory lithophile excess as well as an iron deficiency. In addition, the lunar surface is characterized by refractory siderophile depletions. The combination of these properties appears to require a previous stage of differentiation in a planetary body or bodies. Siderophile and chalcolphile depletions and dispersions in eucrites suggest that these bodies are not necessarily large. Possible mechanisms of lunar formation include impacting of a very large body into the earth; tidal disruption of sizeable differentiated planetesimals by the earth; and selective capture of differentiated planetesimal material by small moonlets. Each mechanism has its difficulties; the major unknown affecting all of them is the size distribution of planetesimals.

Reconciliation of the excess 176Hf conundrum in meteorites: Recent disturbances of the Lu-Hf and Sm-Nd isotope systematics

NASA Astrophysics Data System (ADS)

Bast, Rebecca; Scherer, Erik E.; Sprung, Peter; Mezger, Klaus; Fischer-Gödde, Mario; Taetz, Stephan; Böhnke, Mischa; Schmid-Beurmann, Hinrich; Münker, Carsten; Kleine, Thorsten; Srinivasan, Gopalan

2017-09-01

The long-lived 176Lu-176Hf and 147Sm-143Nd radioisotope systems are commonly used chronometers, but when applied to meteorites, they can reveal disturbances. Specifically, Lu-Hf isochrons commonly yield dates up to ∼300 Myr older than the solar system and varying initial 176Hf/177Hf values. We investigated this problem by attempting to construct mineral and whole rock isochrons for eucrites and angrites. Meteorites from different parent bodies exhibit similar disturbance features suggesting that a common process is responsible. Minerals scatter away from isochron regressions for both meteorite classes, with low-Hf phases such as plagioclase and olivine typically being most displaced above (or left of) reference isochrons. Relatively Hf-rich pyroxene is less disturbed but still to the point of steepening Lu-Hf errorchrons. Using our Lu-Hf and Sm-Nd data, we tested various Hf and Lu redistribution scenarios and found that decoupling of Lu/Hf from 176Hf/177Hf must postdate the accumulation of significant radiogenic 176Hf. Therefore early irradiation or diffusion cannot explain the excess 176Hf. Instead, disturbed meteorite isochrons are more likely caused by terrestrial weathering, contamination, or common laboratory procedures. The partial dissolution of phosphate minerals may predominantly remove rare earth elements including Lu, leaving relatively immobile and radiogenic Hf behind. Robust Lu-Hf (and improved Sm-Nd) meteorite geochronology will require the development of chemical or physical methods for removing unsupported radiogenic Hf and silicate-hosted terrestrial contaminants without disturbing parent-daughter ratios.

Eucrite Impact Melt NWA 5218 - Evidence for a Large Crater on Vesta

NASA Technical Reports Server (NTRS)

Wittmann, Axel; Hiroi, Takahiro; Ross, Daniel K.; Herrin, Jason S.; Rumble, Douglas, III; Kring, David A.

2011-01-01

Northwest Africa (NWA) 5218 is a 76 g achondrite that is classified as a eucrite [1]. However, an initial classification [2] describes it as a "eucrite shock-melt breccia...(in which) large, partially melted cumulate basalt clasts are set in a shock melt flow...". We explore the petrology of this clast-bearing impact melt rock (Fig. 1), which could be a characteristic lithology at large impact craters on asteroid Vesta [3]. Methods: Optical microscopy, scanning electronmicroscopy, and Raman spectroscopy were used on a thin section (Fig. 1) for petrographic characterization. The impact melt composition was determined by 20 m diameter defocused-beam analyses with a Cameca SX-100 electron microprobe. The data from 97 spots were corrected for mineral density effects [4]. Constituent mineral phases were analyzed with a focusedbeam. Bidirectonal visible and near-infrared (VNIR) and biconical FT-IR reflectance spectra were measured on the surface of a sample slab on its central melt area and on an eucrite clast, and from 125-500 m and <125 m powders of melt. Results: General petrography: The sample specimen is a coherent, medium dark-grey (N4), melt rock. The thin section captures a central, subophitic-textured melt that contains 1 cm to tens of m-size subangular to rounded, variably-shocked eucrite clasts. Clasts >100 m are coarse-grained with equigranular 1 mm size plagioclase, quartz, and clinopyroxene (Fig. 1). Single crystals of chromite, ilmenite, zircon, Ca-Mg phosphate, Fe-metal, and troilite are embedded in the melt. Polymineralic clasts are mostly compositionally similar to the above mentioned larger clasts but scarce granulitic fragments are observed as well.

Igneous lithologies on asteroid (4) Vesta mapped using gamma-ray and neutron data

NASA Astrophysics Data System (ADS)

Beck, Andrew W.; Lawrence, David J.; Peplowski, Patrick N.; Viviano-Beck, Christina E.; Prettyman, Thomas H.; McCoy, Timothy J.; McSween, Harry Y.; Yamashita, Naoyuki

2017-04-01

We use data collected by the Dawn Gamma-Ray and Neutron Detector (GRaND) at Vesta to map compositions corresponding to nearly pure igneous lithologies in the howardite, eucrite, diogenite (HED) meteorite clan (samples likely from Vesta). At the ∼300-km spatial scale of GRaND measurements, basaltic eucrite occurs on only 3% of the surface, whereas cumulate eucrite and orthopyroxenitic diogenite are not detected. The basaltic eucrite region is generally coincident with an area of the surface with thick regolith, elevated H, and moderate crater density, and may represent the best compositional sample of primordial vestan crust. We observe an absence of pure orthopyroxenitic diogenite terrains in the Rheasilvia basin and its ejecta, an observation corroborated by VIR (0.1%), which suggests the south-polar crust was a polymict mixture of igneous lithologies (howardite) at the time of the Rheasilvia impact, or was a thick basaltic eucrite crust with heterogeneously distributed orthopyroxenitic diogenite plutons. The most dominant igneous composition detected (11% of the surface) corresponds to one of the least-abundant igneous lithologies in the HED meteorite collection, the Yamato Type B diogenites (plagioclase-bearing pyroxenites). The distribution of Type B diogenite is spatially correlated with post-Rheasilvia craters in the north-polar region that are in close proximity to the Rheasilvia basin antipode. This suggests that north-polar Type B plutonism may have been associated with the Rheasilvia impact event. We propose that this was either through 1) uplift of pre-existing plutons at the antipode through focusing of Rheasilvia impact stress, or 2) Rheasilvia impact antipodal crustal melting, creating magmas that underwent fractionation to produce Type B plutons.

26Al- 26Mg dating of asteroidal magmatism in the young Solar System

NASA Astrophysics Data System (ADS)

Schiller, Martin; Baker, Joel A.; Bizzarro, Martin

2010-08-01

We present high-precision Mg isotope data for most classes of basaltic meteorites including eucrites, mesosiderite silicate clasts, angrites and the ungrouped Northwest Africa (NWA) 2976 measured by pseudo-high-resolution multiple-collector inductively coupled plasma mass spectrometry and utilising improved techniques for chemical purification of Mg. With the exception of the angrites Angra dos Reis, Lewis Cliff (LEW) 86010, NWA 1296 and NWA 2999 and the diogenite Bilanga, which have either been shown to have young ages by other dating techniques or have low Al/Mg ratios, all bulk samples of basaltic meteorites have 26Mg excesses ( δ26Mg=+0.0135 to +0.0392‰). The 26Mg excesses cannot be explained by analytical artefacts, cosmogenic effects or heterogeneity of initial 26Al/ 27Al, Al/Mg ratios or Mg isotopes in asteroidal parent bodies as compared to Earth or chondrites. The 26Mg excesses record asteroidal melting and formation of basaltic magmas with super-chondritic Al/Mg and confirm that radioactive decay of short-lived 26Al was the primary heat source that melted planetesimals. Model 26Al- 26Mg ages for magmatism on the eucrite/mesosiderite, angrite and NWA 2976 parent bodies are 2.6-3.2, 3.9-4.1 and 3.5 Myr, respectively, after formation of calcium-aluminium-rich inclusions (CAIs). However, the validity of these model ages depends on whether the elevated Al/Mg ratios of basaltic meteorites result from magma ocean evolution on asteroids through fractional crystallisation or directly during partial melting. Mineral isochrons for the angrites Sahara (Sah) 99555 and D'Orbigny, and NWA 2976, yield ages of 5.06-0.05+0.06Myr and 4.86-0.09+0.10Myr, respectively, after CAI formation. Both isochrons have elevated initial δ26Mg values. Given the brecciated and equilibrated texture of NWA 2976 it is probable that its isochron age and elevated initial δ26Mg(+0.0175±0.0034‰) reflects thermal resetting during an impact event and slow cooling on its parent body. However, in the case of the angrites the marginally elevated initial δ26Mg(+0.0068±0.0058‰) may reflect either δ26Mg ingrowth in a magma ocean prior to eruption and crystallisation or in an older igneous protolith with super-chondritic Al/Mg prior to impact melting and crystallisation of these angrites, or partial internal re-equilibration of Mg isotopes after crystallisation. 26Al- 26Mg model ages and an olivine + pyroxene + whole rock isochron for the angrites Sah 99555 and D'Orbigny are in good agreement with age constraints from 53Mn- 53Cr and 182Hf- 182W short-lived chronometers, suggesting that the 26Al- 26Mg feldspar-controlled isochron ages for these angrites may be compromised by the partial resetting of feldspar Mg isotope systematics. Even when age constraints from the 26Al- 26Mg angrite model ages or the mafic mineral + whole rock isochron are considered, the relative time difference between Sah 99555/D'Orbigny crystallisation and CAI formation cannot be reconciled with Pb-Pb ages for Sah 99555/D'Orbigny and CAIs, which are ca. 1.0 Myr too old (angrites) or too young (CAIs) for reasons that are not clear. This discrepancy might indicate that 26Al was markedly lower (ca. 40%) in the planetesimal- and planet-forming regions of the proto-planetary disc as compared to CAIs, or that CAI Pb-Pb ages may not accurately date CAI formation, which might be better dated by the 182Hf- 182W and 26Al- 26Mg chronometers as 4568.3±0.7 (Burkhardt et al., 2008) and 4568.5±0.3Ma (herein), respectively, when mapped onto an absolute timescale using Pb-Pb ages for angrites.

Stable Nd isotope variations in the inner Solar System: The effect of sulfide during differentiation?

NASA Astrophysics Data System (ADS)

McCoy-West, A.

2017-12-01

Radiogenic neodymium isotopes have been widely used in studies of planetary accretion to constrain the timescales of early planetary differention [1]. Whereas stable isotope varitaions potentially provide information on the the processes that occur during planet formation. Experimental work suggests that the Earth's core contains a significant proportion of sulfide [2], and recent experimental work shows that under reducing conditions sulfide can incorporate substantial quantities of refractory lithophile elements [including Nd; 3]. If planetary embroyos also contain sulfide-rich cores, Nd stable isotopes have the potential to trace this sulfide segregation event in highly reduced environments, because there is a significant contrast in bonding environment between sulfide and silicate, where heavy isotopes should be preferentially incorporated into high force-constant bonds involving REE3+ (i.e. the silicate mantle). Here we present 146Nd/144Nd data, obtained using a double spike TIMS technique, for a range of planetary bodies formed at variable oxidation states including samples from the Moon, Mars, the asteriod 4Vesta and the Angrite and Aubrite parent bodies. Analyses of chondritic meteorites and terrestrial igneous rocks indicate that the Earth has a Nd stable isotope composition that is indistinguishable from that of chondrites [4]. Eucrites and martian meteorites also have compositons within error of the chondritic average. Significantly more variabilty is observed in the low concentration lunar samples and diogienite meteorites with Δ146Nd = 0.16‰. Preliminary results suggest that the Nd stable isotope composition of oxidised planetary bodies are homogeneous and modifications are the result of subordinate magmatic processes. [1] Boyet & Carlson, Science 309, 576 (2005) [2] Labidi et al. Nature 501, 208 (2013); [3] Wohlers &Wood, Nature 520, 337 (2015); [4] McCoy-West et al. Goldschmidt Ab. 429 (2017).

A Classification Table for Achondrites

NASA Technical Reports Server (NTRS)

Chennaoui-Aoudjehane, H.; Larouci, N.; Jambon, A.; Mittlefehldt, D. W.

2014-01-01

Classifying chondrites is relatively easy and the criteria are well documented. It is based on mineral compositions, textural characteristics and more recently, magnetic susceptibility. It can be more difficult to classify achondrites, especially those that are very similar to terrestrial igneous rocks, because mineralogical, textural and compositional properties can be quite variable. Achondrites contain essentially olivine, pyroxenes, plagioclases, oxides, sulphides and accessory minerals. Their origin is attributed to differentiated parents bodies: large asteroids (Vesta); planets (Mars); a satellite (the Moon); and numerous asteroids of unknown size. In most cases, achondrites are not eye witnessed falls and some do not have fusion crust. Because of the mineralogical and magnetic susceptibility similarity with terrestrial igneous rocks for some achondrites, it can be difficult for classifiers to confirm their extra-terrestrial origin. We -as classifiers of meteorites- are confronted with this problem with every suspected achondrite we receive for identification. We are developing a "grid" of classification to provide an easier approach for initial classification. We use simple but reproducible criteria based on mineralogical, petrological and geochemical studies. We presented the classes: acapulcoites, lodranites, winonaites and Martian meteorites (shergottite, chassignites, nakhlites). In this work we are completing the classification table by including the groups: angrites, aubrites, brachinites, ureilites, HED (howardites, eucrites, and diogenites), lunar meteorites, pallasites and mesosiderites. Iron meteorites are not presented in this abstract.

The S(IV)-type Asteroids as Ordinary Chondrite Parent Body Candidates: Implications for the Completeness of the Meteorite Sample of Asteroids

NASA Astrophysics Data System (ADS)

Gaffey, M. J.

1995-09-01

The discrepancy between the abundance of ordinary chondrites (OCs) among the meteorites and the rarity of unambiguously similar assemblages in the asteroid belt has been a major point of discussion within and between the asteroid and meteorite communities. Various resolutions to this apparent paradox have been proposed [e.g., 1-5], including: 1) interpretations of S-type asteroid spectra are incorrect due to space weathering effects; 2) ordinary chondrites derive from a few rare but favorably situated parent bodies; 3) OCs come from a residual population of small unheated mainbelt asteroids; 4) shock effects darken OC parent body surfaces disguising them as C-type asteroids, and 5) OCs come from inner solar system planetesimals ejected to the Oort cloud which have been recently perturbed into Earth-crossing orbits. Although none of these possibilities has yet been rigorously excluded, recent investigations suggest that the resolution of the apparent paradox lies in some combination of the first three options. For option 3, the discovery of a small mainbelt asteroid with an OC-like spectrum indicates OC-assemblages among the smaller mainbelt asteroids [6], although their abundance is still low in the current sample [7]. For option 2, the mineralogical survey indicated that while most S-asteroids could be rigorously excluded on mineralogical criteria, the S(IV) subtype of this class has silicate compositions within the OC range [8]. The S(IV)-objects are concentrated near the 3:1 secular resonance at 2.5 AU providing an efficient escape into Earth-crossing orbits. Unfortunately for a simple resolution of the OC parent body question, S(IV) spectra still exhibit weaker silicate features and redder spectral slopes than OC assemblages. Although significant uncertainties remain, optical alteration of asteroid surfaces interpreted from the Galileo images of Ida and Gaspra may reconcile the mismatch between OC and S(IV) spectra [option 1]. Although only a subset of the S(IV) objects are viable OC-parent bodies [3 Juno, 6 Hebe, and 7 Iris are the leading candidates], their proximity to the 3:1 chaotic zone would allow them to contribute a significant portion of the ordinary chondrites. In particular, dynamical models suggest that Hebe should be a major contributor to the terrestrial meteorite flux [9]. Each leading contender is currently undergoing detailed spectral evaluation as a potential OC source. From both asteroid observational constraints and from chemical and isotopic studies of meteorites, the ordinary chondrites appear to represent an extensive and relatively complete (by meteoritic standards) sample of a few asteroid source bodies. In a similar fashion, the Howardite-Eucrite-Diogenite suite sample a single primary parent body (Vesta) and are over-represented in meteorite collections due to a fortuitous (and temporary on a solar system timescale) emplacement of Vesta ejecta fragments close to the 3:1 resonance. This suggests that the particular value of the ordinary chondrites lies in the good sample provided for each source body rather than as representatives of an abundant asteroid type. Acknowledgments: Various portions of this research were supported by NASA Planetary Geology and Geophysics grant NAGW-642 and NSF Planetary Astronomy grant AST-9012180. References: [1] Wetherill G. W. and Chapman C. R. (1988) in Meteorites and the Early Solar System, pp. 35-67, Univ. of Arizona. [2] Bell J. F. et al. (1989) in Asteroids II, pp. 921-945, Univ. of Arizona. [3] Gaffey M. J. et al. (1989) in Asteroids II, pp. 98-127, Univ. of Arizona. [4] Britt D. T. and Pieters C. M. (1991) LPS XXII, 141-142. [5] Gaffey M. J. (1984) Icarus, 60, 83-114. [6] Binzel R. P. et al. (1993) Science, 262, 1541-1543. [7] Shui X. et al. (1995) Icarus, 115, 1-35. [8] Gaffey M. J. et al. (1993) Icarus, 106, 573-602. [9] Farinella P. et al. (1993) Icarus, 101, 174-187.

The Complicated Geologic History of Asteroid 4 Vesta

NASA Astrophysics Data System (ADS)

Taylor, G. J.

2009-06-01

Planetary scientists are pretty sure that almost all of the HED meteorites come from the fourth-largest asteroid, 4 Vesta. HED stands for the three types of rocks that make up the group. As cosmochemists have studied the meteorites over the years, their view of the geologic history of the asteroid has become progressively more complicated. Jean-Alix Barrat and Marcel Bohn (CNRS and University of Brest, France), Philippe Gillet (CNRS and Ecole Normale Supérieure de Lyon, France), and Akira Yamaguchi (National Institute of Polar Research, Tokyo, Japan) have found that Vesta is even more complicated--and interesting--than we thought. Barrat and his colleagues analyzed impact-produced glass spherules and fragments in several howardites (mixtures of the two other main types, eucrites and diogenites). Not surprisingly, most of the glasses have compositions similar to eucrites, which are basalts, or mixtures of them with diogenites, but a few are surprisingly rich in silicon and potassium (expressed as the percentages of SiO2 and K2O, respectively). In fact, the concentrations of these oxides are similar to granites, compositionally far from basalt. Their manufacture requires extensive crystallization of magma. Combined with a more subtle variation among the basalts, the emerging picture is one that includes formation of a basaltic crust, partial melting of parts of the crust, mixing of those melts with some (not all) magmas as they migrated through the crust, and extensive crystallization of magma bodies to produce residual magma resembling granites. On top of that, Vestan rocks were thermally metamorphosed and battered and mixed by impacts. A pretty complicated little planetary body!

Textural variations and impact history of the Millbillillie eucrite

NASA Technical Reports Server (NTRS)

Yamaguchi, Akira; Takeda, Hiroshi; Bogard, Donald D.; Garrison, Daniel

1994-01-01

We have investigated 10 new specimens of the Millbillillie eucrite to study its textures and mineral compositions by electron probe microanalyser and scanning electron microscope. Although originally described as having fine-grained texture, the new specimens show diversity of texture. The compositions (Mg/Fe ratios) of the host pigeonites and augite lamellae are homogeneous, respectively, in spite of the textural variation. In addition to their chemical homogeneity, pyroxenes in coarse and fine-grained clasts are partly inverted to orthopyroxene. Chemical zoning of plagioclase during crystal growth is preserved. This eucrite includes areas of granulitic breccias and impact melts. Large scale textures show a subparallel layering suggesting incomplete mixing and deposition of impact melt and lithic fragments. An Ar-39-Ar-40 age determination for a coarse-grained clast indicates a strong degassing event at 3.55 +/- 0.02 Ga. We conclude that Millbillillie is among the most equilibriated eucrites produced by thermal annealing after impact brecciation. According to the classificcation of impact breccias, Millbillillie can be classified as a mixture of granulitic breccias and impact melts. The last significant thermal event is characterized by network-like glassy veins that run through clasts and matrices. Consideration of textual observations and requirements for Ar-degassing suggests that the Ar-39-Ar-40 age could in principle date either the earlier brecciation and annealing event or the event which produced the veins.

Volatile Content of 4-Vesta: Evidence from Unequilibrated Eucrites

NASA Technical Reports Server (NTRS)

Sarafian, A. R.; Nielsen, S. G.; Marschall, H. R.; Gaetani, G. A.; Hauri, E. H.; Righter, K.; Berger, E. L.

2017-01-01

Eucrites are a class of basaltic meteorites that, along with the howardites and diogenites, likely derive from the asteroid 4-Vesta. This asteroid is depleted in moderately volatile elements relative to the Earth and carbonaceous chondrites. Extrapolation of this depletion trend predicts that bulk silicate 4-Vesta (BSV) contains at most 250-1000 µg/g H2O, which is approximately a factor of two lower than the H2O content of Earth. To obtain more accurate H2O and F estimates for BSV, we examined four unequilibrated antarctic meteorites, Yamato(Y)-793548, Y-82210, Y-75011, and Y-74450, by EPMA and SIMS. Pyroxenes contain MgO-rich cores and FeO-rich rims, consistent with primary magmatic zoning. Volatile concentrations generally follow patterns expected for growth zoning with lower values in the cores and higher in the rims. These features indicate that thermal metamorphism and other post-crystallization processes did not significantly perturb the volatile contents of these unequilibrated eucrite pyroxenes. We used these data to derive best estimates for the BSV H2O and F content based on experimentally determined pyroxene-melt partition coefficients and models for magma generation on Vesta. In addition, we measured D/H in the early crystallizing pyroxenes and late crystallzing apatites. We find that the D/H of pyroxene and apatite are within error of one another as well as previous measurements of apatite in equilibrated eucrites. These results imply that degassing was minimal or did not fractionate D/H. Degassing may have been limited if eucrites were shallowly emplaced sills or dykes, or the total H2O content of the magmas was too low for vapor saturation. An alternative mechanism for limited D/H fractionation is that degassing did occur, but the H2/H2O of the exsolved vapor was approximately 15:85, as predicted from experiments.

Post-igneous redistribution of components in eucrites

NASA Technical Reports Server (NTRS)

Phinney, W. C.; Lindstrom, D. J.; Mittlefehldt, D. W.; Martinez, R. R.

1993-01-01

In our analyses, we utilize a microdrilling technique that removes 40 to 100 micron diameter cores from mineral grains in thin sections analyzed by microprobe. The cores are then analyzed by INAA using the technique of Lindstrom. Three eucrites were selected for application of this analytical technique: monomict breccias Pasamonte and Stannern and unbrecciated EET90020. Pasamonte is among the most unequilibrated of the eucrites on the basis of zoning in pyroxenes and is considered to be an igneous rock not significantly affected by metamorphism. Stannern has igneous texture but its pyroxenes indicate some re-equilibration, although little, if any, recrystallization. EET90020 has a granulite texture and has been substantially recrystallized. Our sample of Pasamonte contains several clasts of different grain sizes ranging from glass to fine grained with diabasic texture containing lathy plagioclase, unexsolved pigeonite, and mesostasis. Cores were taken of the glass and from minerals and mesostases in six lithic clasts which normally allowed sampling of more than one phase per clast. Our sample of Stannern is also a breccia but with little difference in grain size between clasts and matrix. The plagioclase and pigeonite are blocky, twinned, and exsolved and coexist with a bit of mesostasis. Cores were taken of plagioclase and pigeonite with no attempt to distinguish separate clasts. EET90020 is a granular mixture of twinned plagioclase and pigeonite having rather uniform size and many triple junctions. Several cores were taken of both phases. Both clear and cloudy grains of plagioclase and pyroxene were sampled in all three eucrites.

Dating Howardite Melt Clasts: Evidence for an Extended Vestan Bombardment?

NASA Technical Reports Server (NTRS)

Cartwright, J. A.; Hodges, K. V.; Wadhwa, M.; Mittlefehldt, D. W.

2016-01-01

Howardites are polymict breccias that, together with eucrites and diogenites (HED), likely originate from the vestan surface (regolith/ megaregolith), and display a heterogeneous distribution of eucritic and diogenitic material. Melt clasts are also present alongside other regolithic features within howardites, and are noteworthy for their compositional variability and appearance. Melt clasts formed by impact events provide a snapshot of the timings and conditions of surface gardening and bombardment on the vestan surface. By dating such clasts, we aim to better constrain the timings of impact events on Vesta, and to establish whether the impact flux in the asteroid belt was similar to that on the Moon. As the Moon is used as the basis for characterising impact models of the inner solar system, it is necessary to verify that apparent wide-scale events are seen in other planetary bodies. In particular, the observed clustering of Apollo melt clast ages between 3.8-4.0 Ga has led to two hypotheses: 1) The Moon was subjected to a sudden event - 'Lunar Cataclysm' or period of 'Late Heavy Bombardment' (LHB), 2) The age cluster represents the end of an epoch of declining bombardment or 'Heavy Bombardment. No consensus has emerged regarding one or other hypothesis. We are testing these hypotheses by seeking evidence for such events in materials other than those derived from the Moon.

Mineralogy of dark clasts in primitive versus differentiated meteorites

NASA Technical Reports Server (NTRS)

Zolensky, M. E.; Weisberg, M. K.; Barrett, R. A.; Prinz, M.

1993-01-01

The presence of dark lithic clasts within meteorites can provide information concerning asteroidal regolith processes, the extent of interactions between asteroids, and the relationship between meteorite types, micrometeorites, and interplanetary dust particles. Accordingly, we have been seeking and characterizing dark clasts found within carbonaceous chondrites, unequilibrated ordinary chondrites, howardites, and eucrites. We find that unequilibrated chondrites in this study contain fine-grained, anhydrous unequilibrated inclusions, while the howardites often contain inclusions from geochemically processed, hydrous asteroids (type 1 and 2 carbonaceous chondrites). Eucrites and howardities contain unusual clasts, not easily classified.

Ar-39-Ar-40 Age Dating Of Two Angrites and Two Brachinites

NASA Technical Reports Server (NTRS)

Garrison, Daniel; Bogard, Donald

2003-01-01

Angrites are a rare group (approximately 7 known) of igneous meteorites with basalt-like composition, which probably derive from a relatively small parent body that differs from those of other igneous meteorites. Angrites show evidence for extinct Mn-53, Sm-146, and Pu-244, and precise U-Pb, and Pb-Pb ages of 4.558 Gyr for two angrites define the time of early parent body differentiation. The Sm-147-Nd-143 ages of two angrites range between 4.53 +/- 0.04 and 4.56 +/- 0.04 Gyr, but no Ar-39-Ar-40 or Rb-Sr ages have been reported. Most angrites show no evidence for either shock brecciation or metamorphism. Brachinites are another very rare group' of differentiated meteorites consisting primarily of olivine, with minor augite, chromite, Fe-sulfides, and sometimes plagioclase and opx. Presence of excess Xe-129 and excess Cr53 from decay of Mn-53 in some brachinites indicate that they also formed very early. Brachinite petrogenesis is poorly defined. They may be igneous cumulates or metamorphic products of chondritic-like starting material. If after their formation, angrites and brachinites cooled quickly with minimal subsequent heating, then one might expect them to show uniquely old K-Ar ages, at least in comparison to other differentiated meteorites such as eucrites and mesosiderites. Most angrites and brachinites contain very little, if any K-feldspar, which has deterred measurements of their Ar-Ar ages. We made Ar-39-Ar-40 analyses on two angrites, LEW86010 (metamorphosed) and D'Orbigny, and on two brachinites, EET99402 and Brachina. All are finds. Any feldspar in angrites is highly calcic, with expected K concentrations of <100 ppm. We selected LEW86010 and D'Orbigny because they have been the objects of several other studies and because chemical analyses suggested [K] was approximately 70 ppm in both meteorites. Brachina contains approximately 9.9% plagioclase of higher K-content than angrites, and EET99402 is estimated to contain approximately 5% K-poor plagioclase. Other brachinites contain little to no feldspar. We have successfully measured Ar-Ar ages on a few meteorites and lunar anorthosites with [K] <100 ppm.

Neutron absorption constraints on the composition of 4 Vesta

USGS Publications Warehouse

Prettyman, Thomas H.; Mittlefehldt, David W.; Yamashita, Naoyuki; Beck, Andrew W.; Feldman, William C.; Hendricks, John S.; Lawrence, David J.; McCoy, Timothy J.; McSween, Harry Y.; Paplowski, Patrick N.; Reedy, Robert C.; Toplis, Michael J.; Le Corre, Lucille; Mizzon, Hugau; Reddy, Vishnu; Titus, Timothy N.; Raymond, Carol A.; Russell, Christopher T.

2013-01-01

Global maps of the macroscopic thermal neutron absorption cross section of Vesta's regolith by the Gamma Ray and Neutron Detector (GRaND) on board the NASA Dawn spacecraft provide constraints on the abundance and distribution of Fe, Ca, Al, Mg, and other rock-forming elements. From a circular, polar low-altitude mapping orbit, GRaND sampled the regolith to decimeter depths with a spatial resolution of about 300 km. At this spatial scale, the variation in neutron absorption is about seven times lower than that of the Moon. The observed variation is consistent with the range of absorption for howardite whole-rock compositions, which further supports the connection between Vesta and the howardite, eucrite, and diogenite meteorites. We find a strong correlation between neutron absorption and the percentage of eucritic materials in howardites and polymict breccias, which enables petrologic mapping of Vesta's surface. The distribution of basaltic eucrite and diogenite determined from neutron absorption measurements is qualitatively similar to that indicated by visible and near infrared spectroscopy. The Rheasilvia basin and ejecta blanket has relatively low absorption, consistent with Mg-rich orthopyroxene. Based on a combination of Fe and neutron absorption measurements, olivine-rich lithologies are not detected on the spatial scales sampled by GRaND. The sensitivity of GRaND to the presence of mantle material is described and implications for the absence of an olivine signature are discussed. High absorption values found in Vesta's “dark” hemisphere, where exogenic hydrogen has accumulated, indicate that this region is richer in basaltic eucrite, representative of Vesta's ancient upper crust.

Neutron absorption constraints on the composition of 4 Vesta

NASA Astrophysics Data System (ADS)

Prettyman, Thomas H.; Mittlefehldt, David W.; Yamashita, Naoyuki; Beck, Andrew W.; Feldman, William C.; Hendricks, John S.; Lawrence, David J.; McCoy, Timothy J.; McSween, Harry Y.; Peplowski, Patrick N.; Reedy, Robert C.; Toplis, Michael J.; Corre, Lucille; Mizzon, Hugau; Reddy, Vishnu; Titus, Timothy N.; Raymond, Carol A.; Russell, Christopher T.

2013-11-01

Global maps of the macroscopic thermal neutron absorption cross section of Vesta's regolith by the Gamma Ray and Neutron Detector (GRaND) on board the NASA Dawn spacecraft provide constraints on the abundance and distribution of Fe, Ca, Al, Mg, and other rock-forming elements. From a circular, polar low-altitude mapping orbit, GRaND sampled the regolith to decimeter depths with a spatial resolution of about 300 km. At this spatial scale, the variation in neutron absorption is about seven times lower than that of the Moon. The observed variation is consistent with the range of absorption for howardite whole-rock compositions, which further supports the connection between Vesta and the howardite, eucrite, and diogenite meteorites. We find a strong correlation between neutron absorption and the percentage of eucritic materials in howardites and polymict breccias, which enables petrologic mapping of Vesta's surface. The distribution of basaltic eucrite and diogenite determined from neutron absorption measurements is qualitatively similar to that indicated by visible and near infrared spectroscopy. The Rheasilvia basin and ejecta blanket has relatively low absorption, consistent with Mg-rich orthopyroxene. Based on a combination of Fe and neutron absorption measurements, olivine-rich lithologies are not detected on the spatial scales sampled by GRaND. The sensitivity of GRaND to the presence of mantle material is described and implications for the absence of an olivine signature are discussed. High absorption values found in Vesta's "dark" hemisphere, where exogenic hydrogen has accumulated, indicate that this region is richer in basaltic eucrite, representative of Vesta's ancient upper crust.

Preliminary Iron Distribution on Vesta

NASA Technical Reports Server (NTRS)

Mittlefehldt, David W.; Mittlefehldt, David W.

2013-01-01

The distribution of iron on the surface of the asteroid Vesta was investigated using Dawn's Gamma Ray and Neutron Detector (GRaND) [1,2]. Iron varies predictably with rock type for the howardite, eucrite, and diogenite (HED) meteorites, thought to be representative of Vesta. The abundance of Fe in howardites ranges from about 12 to 15 wt.%. Basaltic eucrites have the highest abundance, whereas, lower crustal and upper mantle materials (cumulate eucrites and diogenites) have the lowest, and howardites are intermediate [3]. We have completed a mapping study of 7.6 MeV gamma rays produced by neutron capture by Fe as measured by the bismuth germanate (BGO) detector of GRaND [1]. The procedures to determine Fe counting rates are presented in detail here, along with a preliminary distribution map, constituting the necessary initial step to quantification of Fe abundances. We find that the global distribution of Fe counting rates is generally consistent with independent mineralogical and compositional inferences obtained by other instruments on Dawn such as measurements of pyroxene absorption bands by the Visual and Infrared Spectrometer (VIR) [4] and Framing Camera (FC) [5] and neutron absorption measurements by GRaND [6].

Core Formation on Asteroid 4 Vesta: Iron Rain in a Silicate Magma Ocean

NASA Technical Reports Server (NTRS)

Kiefer, Walter S.; Mittlefehldt, David W.

2017-01-01

Geochemical observations of the eucrite and diogenite meteorites, together with observations made by NASA's Dawn spacecraft, suggest that Vesta resembles H chondrites in bulk chemical composition, possibly with about 25% of a CM-chondrite like composition added in. For this model, the core is 15% by mass (or 8 volume %) of the asteroid. The abundances of moderately siderophile elements (Ni, Co, Mo, W, and P) in eucrites require that essentially all of the metallic phase in Vesta segregated to form a core prior to eucrite solidification. Melting in the Fe-Ni-S system begins at a cotectic temperature of 940 deg. C. Only about 40% of the total metal phase, or 3-4 volume % of Vesta, melts prior to the onset of silicate melting. Liquid iron in solid silicate initially forms isolated pockets of melt; connected melt channels, which are necessary if the metal is to segregate from the silicate, are only possible when the metal phase exceeds about 5 volume %. Thus, metal segregation to form a core does not occur prior to the onset of silicate melting.

Differentiation of Asteroid 4 Vesta: Core Formation by Iron Rain in a Silicate Magma Ocean

NASA Technical Reports Server (NTRS)

Kiefer, Walter S.; Mittlefehldt, David W.

2017-01-01

Geochemical observations of the eucrite and diogenite meteorites, together with observations made by NASA's Dawn spacecraft while orbiting asteroid 4 Vesta, suggest that Vesta resembles H chondrites in bulk chemical composition, possible with about 25 percent of a CM-chondrite like composition added in. For this model, the core is 15 percent by mass (or 8 percent by volume) of the asteroid, with a composition of 73.7 percent by weight Fe, 16.0 percent by weight S, and 10.3 percent by weight Ni. The abundances of moderately siderophile elements (Ni, Co, Mo, W, and P) in eucrites require that essentially all of the metallic phase in Vesta segregated to form a core prior to eucrite solidification. The combination of the melting phase relationships for the silicate and metal phases, together with the moderately siderophile element concentrations together require that complete melting of the metal phase occurred (temperature is greater than1350 degrees Centigrade), along with substantial (greater than 40 percent) melting of the silicate material. Thus, core formation on Vesta occurs as iron rain sinking through a silicate magma ocean.

Modelling the Thermal History of Asteroid 4 Vesta

NASA Technical Reports Server (NTRS)

Solano, James M.; Kiefer, W. S.; Mittlefehldt, D. W.

2012-01-01

The asteroid 4 Vesta is widely thought to be the source of the HED (Howardite, Eucrite and Diogenite) meteorites, with this link supported by spectroscopic and dynamical studies. The availability of the HED meteorites for study and the new data being gained from the Dawn mission provides an excellent opportunity to investigate Vesta s history. In this study, modelling of Vesta has been undertaken to investigate its evolution from an unconsolidated chondritic body to a differentiated body with an iron core. In contrast to previous modelling, both heat and mass transfer are considered as coupled processes. This work draws on models of melt segregation in terrestrial environments to inform the evolution of Vesta into the differentiated body observed today. In order for a core to form in this body, a separation of the metallic iron from the silicates must take place. Temperatures in excess of the solidus temperatures for the Fe-FeS system and the silicates are therefore required. Thermal modelling has shown accretion before 2Myr leads to temperatures in excess of the silicate solidus.

An ancient core dynamo in asteroid Vesta.

PubMed

Fu, Roger R; Weiss, Benjamin P; Shuster, David L; Gattacceca, Jérôme; Grove, Timothy L; Suavet, Clément; Lima, Eduardo A; Li, Luyao; Kuan, Aaron T

2012-10-12

The asteroid Vesta is the smallest known planetary body that has experienced large-scale igneous differentiation. However, it has been previously uncertain whether Vesta and similarly sized planetesimals formed advecting metallic cores and dynamo magnetic fields. Here we show that remanent magnetization in the eucrite meteorite Allan Hills A81001 formed during cooling on Vesta 3.69 billion years ago in a surface magnetic field of at least 2 microteslas. This field most likely originated from crustal remanence produced by an earlier dynamo, suggesting that Vesta formed an advecting liquid metallic core. Furthermore, the inferred present-day crustal fields can account for the lack of solar wind ion-generated space weathering effects on Vesta.

High-pressure minerals in eucrite suggest a small source crater on Vesta

PubMed Central

Pang, Run-Lian; Zhang, Ai-Cheng; Wang, Shu-Zhou; Wang, Ru-Cheng; Yurimoto, Hisayoshi

2016-01-01

High-pressure minerals in meteorites are important records of shock events that have affected the surfaces of planets and asteroids. A widespread distribution of impact craters has been observed on the Vestan surface. However, very few high-pressure minerals have been discovered in Howardite-Eucrite-Diogenite (HED) meteorites. Here we present the first evidence of tissintite, vacancy-rich clinopyroxene, and super-silicic garnet in the eucrite Northwest Africa (NWA) 8003. Combined with coesite and stishovite, the presence of these high-pressure minerals and their chemical compositions reveal that solidification of melt veins in NWA 8003 began at a pressure of >~10 GPa and ceased when the pressure dropped to <~8.5 GPa. The shock temperature in the melt veins exceeded 1900 °C. Simulation results show that shock events that create impact craters of ~3 km in diameter (subject to a factor of 2 uncertainty) are associated with sufficiently high pressures to account for the occurrence of the high-pressure minerals observed in NWA 8003. This indicates that HED meteorites containing similar high-pressure minerals should be observed more frequently than previously thought. PMID:27181381

What heated the parent meteorite planets?

NASA Technical Reports Server (NTRS)

Wood, John A.; Pellas, Paul

1991-01-01

The plausibility of the two most wide discussed mechanisms, decay of short-lived Al-26 and solar wind induction heating, for heating the small planetesimals in which the meteorites formed are examined and shown to have significant problems. The main problem for the Al-26 decay mechanism is the fact that eucritic lavas, melted by the mysterious heating mechanism in some early planetesimal, did not contain enough Al-26 to decay to radiogenic Mg-26 when they erupted to their planetesimal surface and cooled. It is necessary to postulate that the lavas lingered underground while their Al-26 decayed away. The solar wind induction heat concept has the problem that astrophysical evidence has made is seem increasingly unlikely that an intense solar wind flux blew past planetesimals in the early solar system. Instead, it was probably collimated in the direction of the sun's poles by the persistence of the solar nebula during the T Tauri epoch.

Excess Silica Substitution in Plagioclase Grains in the Pasamonte Eucrite

NASA Technical Reports Server (NTRS)

Mittlefehldt, D. W.; Le, L.; Berger, E. L.

2017-01-01

Pasamonte is a clast-rich polymict basaltic breccia with O- and Cr-isotopic compositions that are resolved from those of most eucrites. It is dominated by two mafic clast types: (i) very-fine- to fine-grained, variolitic, subophitic and ophitic basalts, usually containing zoned pyroxenes; and (ii) fine- to medium grained hypidiomorphic-granular and allotriomorphic-granular microgabbros containing pyroxenes composed of augite lamellae in homogeneous pigeonite hosts. Minor clast types are fine-grained impact-melt, mafic-breccia and mafic-granular clasts; coarse matrix mineral fragments include pyroxene, plagioclase, silica, ferroan olivine and ilmenite. Our petrologic studies include determination of plagioclase compositions for the two major clast types and matrix grains, which we report here.

Redetermination of the Sm-Nd Age and Initial (Epsilon)Nd of Lunar Troctolite 76535: Implications for Lunar Crustal Development

NASA Technical Reports Server (NTRS)

Nyquist, Laurence E.; Shih, C.-Y.; Reese, Y. D.

2012-01-01

Lunar troctolite 76535 is an old lunar rock predating the era of the lunar cataclysmic bombardment, but its radiometrially determined ages have been discordant [1-3]. The most recent multi-chronometer study [4] gave preferred ages of 4226+/-35 Ma and 4236+/-15 Ma from a Pb-207/Pb-206 isochron and an U-Pb upper concordia intercept, resp. We derive an age of 4323+/-64 Ma from Sm-Nd data reported by [4] for the bulk rock and three mineral separates. They derived an age of approx.4.38 Ga from combined Rb-Sr data [3,4] by omitting data for olivine separates. Ar-39-Ar-40 ages of approx.4.2 Ga are summarized by [5]. New Sm-147-Nd-143 data presented here give an age of 4335+/-71 Ma in agreement with the Sm-Nd age from [4], whereas Sm-146-Nd-142 data give a model age T(sub LEW) = 4439+/-22 Ma. Further, initial (Epsilon)Nd-143 for 76535 conforms to the Nd-143 evolution expected in an urKREEP [6] reservoir, consistent with inheritance of urKREEP Sm-Nd systematics via assimilation. We show that urKREEP Sm-Nd systematics require the lunar initial (Epsilon)Nd-143 to exceed the Chondritic Uniform Reservoir (CHUR) value [7], but are consistent with evolution from initial (Epsilon)Nd-143 like that of the HED meteorite parent body as defined by a 4557+/-20 Ma internal isochron for the cumulate eucrites Y-980433 and Y- 980318 [8].

Magnesium isotope compositions of Solar System materials determined by double spiking

NASA Astrophysics Data System (ADS)

Hin, R.; Lai, Y. J.; Coath, C.; Elliott, T.

2015-12-01

As a major element, magnesium is of interest for investigating large scale processes governing the formation and evolution of rocky planetary bodies. Determining the Mg isotope composition of the Earth and other planetary bodies has hence been a topic of interest ever since mass-dependent fractionation of 'non-traditional' stable isotopes has been used to study high-temperature processes. Published results, however, suffer from disagreement on the Mg isotope compositions of the Earth and chondrites [1-5], which is attributed to residual matrix effects. Nonetheless, most recent studied have converged towards a homogeneous (chondritic) Mg isotope composition in the Solar System [2-5]. However, in several of the recent studies there is a hint of a systematic difference of about 0.02-0.06‰ in the 26Mg/24Mg isotope compositions of chondrites and Earth. Such difference, however, is only resolvable by taking standard errors, which assumes robust data for homogenous sample sets. The discrepancies between various studies unfortunately undermine the confidence in such robustness and homogeneity. The issues with matrix effects during isotopic analyses can be overcome by using a double spike approach. Such methodology generally requires three isotope ratios to solve for three unknowns, a requirement that cannot be met for Mg. However, using a newly developed approach, we present Mg isotope compositions obtained by critical mixture double spiking. This new approach should allow greater confidence in the robustness of the data and hence enable improvement of. Preliminary data indicate that chondrites have a resolvable ~0.04‰ lighter 26Mg/24Mg than (ultra)mafic rocks from Earth, Mars and the eucrite parent body, which appear indistinguishable from each other. It seems implausible that this difference is caused by magmatic process such as partial melting or crystallisation. More likely, Mg isotopes are fractionated by a non-magmatic process during the formation of planets, e.g. by vapour-condensate fractionation. [1] Wiechert and Halliday, 2007. EPSL 256, 360-371. [2] Bourdon et al., 2010. GCA 74, 5069-5083. [3] Teng et al., 2010. GCA 74, 4150-4166. [4] Chakrabarti and Jacobsen, 2010. EPSl 293, 349-358. [5] Von Strandmann, 2011. GCA 75, 5247-5268.

Sm-Nd and Initial Sr-87/Sr-86 Isotopic Systematics of Asuka 881394 and Cumulate Eucrites Yamato 980318/433 Compared

NASA Technical Reports Server (NTRS)

Nyquist, L. E.; Shih, C-Y; Young, Y. D.; Takeda, H.

2011-01-01

The Asuka 881394 achondrite contains fossil Al-26 and Mn-53 and has a Pb-206/Pb-207 age of 4566.5 +/- 0.2 Ma, the oldest for an achondrite. Recent re-investigation of A881394 yielded revised initial Sm-146/Sm-144 = (9.1 +/- 1.4) x 10(exp -3), a Sm-147-Nd-143 age of 4525 +/- 58 Ma, a Rb-87-Sr-87 age of 4490 +/- 130 Ma, and initial Sr-87/Sr-86 = 0.698991 +/- 19, respectively. The relatively large uncertainties in the Sm-Nd and Rb-Sr ages are due to disturbances of the isotopic systematics of tridymite and other minor phases. A preliminary value for the Sm-147-Nd-143 age of the Yamato 980318 cumulate eucrite of 4560 +/- 150 Ma was refined in later work to 4567 +/- 24 Ma as reported orally at LPSC 35. Similarly, a preliminary value for Sm-146/Sm-144 = (7.7 +/- 1.2) x 10 (exp -3) was refined to (6.0 +/- 0.3) x 10(exp -3). For Yamato 980433, a Sm-147-Nd-143 age of 4542 +/-42 Ma and Sm-146/Sm-144 = (5.7 +/- 0.5) x 10(exp -3) has been reported. Because these two cumulate eucrites are paired, we consider them to represent one igneous rock and present their combined isotopic data here.

Mineralogy, petrology and geochemistry of carbonaceous chondritic clasts in the LEW 85300 polymict eucrite

NASA Technical Reports Server (NTRS)

Zolensky, M. E.; Hewins, R. H.; Mittlefehldt, D. W.; Lindstrom, M. M.; Xiao, X.; Lipschutz, M. E.

1992-01-01

We have performed a detailed petrologic and mineralogic study of two chondritic clasts from the polymict eucrite Lewis Cliff (LEW) 85300, and performed chemical analyses by INAA and RNAA on one of these. Petrologically, the clasts are identified and are composed of dispersed aggregates, chondrules, and chondrule fragments supported by matrix. The aggregates and chondrules are composed of olivine, orthopyroxene, plus some diopside. The matrix consists of fine-grained olivine, and lesser orthopyroxene and augite. Fine-grained saponite is common in the matrix. The bulk major composition of the clast studied by INAA and RNAA shows unusual abundance patterns for lithophile, siderophile and chalcophile elements but is basically chondritic. The INAA/RNAA data preclude assignment of the LEW 85300,15 clast to any commonly accepted group of carbonaceous chondrite.

Rocks from Vesta -- Part 3: Diogenites

NASA Image and Video Library

2011-12-04

These images are of HED howardite, eucrite and diogenite meteorites are a large group of meteorites believed to originate from asteroid Vesta, a hypothesis that is consistent with current Dawn observations.

Rocks from Vesta -- Part 2: Howardites

NASA Image and Video Library

2011-12-03

These images are of HED howardite, eucrite and diogenite meteorites are a large group of meteorites believed to originate from asteroid Vesta, a hypothesis that is consistent with current Dawn observations.

Types and Distribution of Bright Materials in 4 Vesta

NASA Technical Reports Server (NTRS)

Mittlefehldt, D. W.; Li, Jian-Yang; Pieters, C. M.; De Sanctis, M. C.; Schroder, S. E.; Hiesinger, H.; Blewett, D. T.; Russell, C. T.; Raymond, C. A.; Yingst, R. A.

2012-01-01

A strong case can be made that Vesta is the parent asteroid of the howardite, eucrite and diogenite (HED) meteorites [1]. As such, we have over a century of detailed sample analysis experience to call upon when formulating hypotheses regarding plausible lithologic diversity on Vesta. It thus came as a surprise when Dawn s Framing Camera (FC) first revealed distinctly localized materials of exceptionally low and high albedos, often closely associated. To understand the nature and origin of these materials, and how they inform us of the geological evolution of Vesta, task forces began their study. An initial step of the scientific endeavor is to develop a descriptive, non-genetic classification of objects to use as a basis for developing hypotheses and observational campaigns. Here we present a catalog of the types of light-toned deposits and their distribution across Vesta. A companion abstract [2] discusses possible origins of bright materials and the constraints they suggest for vestan geology.

Arruntia Crater: A Rare Window into Vesta’s Northern Hemisphere

NASA Astrophysics Data System (ADS)

Sunshine, Jessica; Cheek, Leah

2015-11-01

One of the intriguing results of the Dawn mission to Vesta was the discovery that the only deposits containing significant olivine, a key mineralogic indicator of primitive materials, occur in two shallow craters in the northern hemisphere. Numerous investigations into these exposures using either the Framing Camera (FC) or the VIR spectrometer typically find similarities between the olivine outcropping in Bellicia’s wall and in the Arruntia ejecta. Our own investigations - using a hybrid VIR-FC approach -suggest an important distinction between the exposures at the two craters. Specifically, we find that the proximal Arruntia ejecta are dominated not by an olivine-rich component (although isolated examples occur), but instead by a more evolved, eucritic component. These interspersed eucritic materials are similar to olivine-rich materials in FC data because both components pull the 1 um band to longer wavelengths. Ultimately, however, they are distinguished by the position and strength of the 2 um band, which is not covered by FC wavelengths. The Arruntia ejecta also appear olivine-like in some parameterizations of VIR spectra for the area, but closer examination of the full spectra at a fine spatial scale clearly suggests the presence of two different materials. Interestingly, the approach used here also reveals a separate diogenitic component in the distal Arruntia ejecta as well as in isolated locations within Arruntia’s wall. Initial evaluation of stratigraphic relationships in the Arruntia ejecta suggest a pre-impact sequence of eucrite -> olivine-rich -> diogenite grading from depth to the shallowest subsurface (although the small size of Arruntia means that this entire assemblage was excavated from no more than a few of kilometers below the surface). These results illustrate two main points: first, that pyroxene-bearing materials rich in olivine are difficult to distinguish from evolved pyroxenes in the absence of full resolution spectroscopy at a fine spatial scale. Second, we find that Arruntia crater is likely a unique location on Vesta where pervasive mechanical gardening has not yet masked the stratigraphic relationships between endmember diogenitic and eucritic components nor olivine-enhancements.

A pristine eucrite-like gabbro from Descartes and its exotic kindred

NASA Technical Reports Server (NTRS)

Marvin, U. B.; Warren, P. H.

1980-01-01

A coarse-grained plagioclase-pyroxene gabbro (61224,6) with a cumulate texture suggestive of a slowly cooled plutonic rock was recovered from the 4-10 mm fraction of an Apollo 16 soil. The rock is uncommonly poor in feldspar and rich in Na for a lunar highlands lithology. Trace element analyses show extremely low siderophile element concentrations which confirm the pristine character indicated by the texture. The composition of 61224,6 is compared with those of 3 other pristine, exceptionally mafic, nonmare gabbros and of certain eucrites. 61224,6 and the three other gabbros have notable chemical differences but share relatively high ratios of Ti/Sm and Sc/Sm which suggest a possible genetic relationship. We conclude that 61224,6 represents a Na-rich cumulate from a layered intrusion within the highlands crust.

Automated Spectral System for Terrain Classification, Mineralogy of Vesta from the Dawn Framing Cameras

NASA Astrophysics Data System (ADS)

Reddy, V.; Le Corre, L.; Nathues, A.; Hall, I.; Gutierrez-Marques, P.; Hoffmann, M.

2011-10-01

The Dawn mission will rendezvous with asteroid (4) Vesta in July 2011. We have developed a set of equations for extracting mean pyroxene chemistry (Ferrosilite and Wollastonite) for classifying terrains on Vesta by using the Dawn Framing Camera (FC) multi-color bands. The Automated Spectral System (ASS) utilizes pseudo-Band I minima to estimate the mean pyroxene chemistry of diogenites, and basaltic eucrites. The mean pyroxene chemistries of cumulate eucrites, and howardites overlap each other on the pyroxene quadrilateral and hence are harder to distinguish. We expect our ASS to carry a bulk of the terrain classification and mineralogy workload utilizing these equations and complement the work of DawnKey (Le Corre et al., 2011, DPS/EPSC 2011). The system will also provide surface mineral chemistry layers that can be used for mapping Vesta's surface.

Investigation of Orthopyroxene Diversity in Howardite Meteorites

NASA Technical Reports Server (NTRS)

Johnson, Kristin N.; Herrin, J. S.; Mittlefehldt, D. W.

2011-01-01

The howardite, eucrite and diogenite (HED) family of meteorites is considered to originate from the asteroid 4-Vesta [1]. Howardites are polymict breccias made mostly of diogenitic and eucritic debris [2], and have recently been divided into two types: regolithic and fragmental [3]. Regolithic howardites have higher noble gas contents due to solar wind exposure, have a greater abundance of impact-produced glass, are richer in siderophile elements, e.g. Ni, and may preferentially have a mixing ratio of eucrite to diogenite of approx.2:1 [3]. The hypothesis is that these characteristics are a result of originating from an ancient, well-mixed regolith [3]. Fragmental howardites, by contract, show less evidence of regolithic processing and are suggested to have originated in more recently formed impact ejecta [3]. Our work aims to evaluate this hypothesis. We have examined the compositional variations of orthopyroxene (diogenite) clasts within eight howardites. We posited that because regolithic howardites sampled a wider range of the asteroid surface, they would contain orthopyroxene fragments with wider ranges in incompatible element contents than would fragmental howardites that sampled fewer diogenitic source rocks. One purpose of developing an additional method to differentiate regolithic and fragmental howardites is to aid in interpretation of data expected from the Dawn mission to 4-Vesta. The Dawn analyses will be of the regolith layers, making an understanding of regolithic meteorites and the processes by which they were formed an important constraint on understanding Dawn data.

Towards a Regolith Maturity Index for Howardites

NASA Technical Reports Server (NTRS)

Mittlefehldt, David W.; Cartwright, J. A.; Herrin, J. S.; Johnson, K. N.

2011-01-01

The Dawn spacecraft has just arrived at asteroid 4 Vesta, parent of the howardite, eucrite and diogenite (HED) meteorites [1], to begin a yearlong surface study from orbit [2]. As Dawn will view a debris-covered surface, understanding the formation and mixing processes for the debris layer will strongly aid surface data interpretations. Howardites are polymict breccias mainly composed of clasts derived from basaltic (eucritic) and orthopy-roxenitic (diogenitic) parent materials [3]. Some howardites are poorly reworked (fragmental howardites) whilst others have been extensively gardened in an active regolith (regolithic howardites) [4]. The latter may represent an ancient, well-mixed regolith, whilst the former may be from more recent ejecta deposits [4]. Due to environmental differences, regolith development on Vesta differs in detail from that on the Moon [4-6]. We have been developing petrological criteria to apply to howardite thin sections to determine their relative regolithic maturity, which we are fine-tuning with comparison to noble gas data [7, 8]. Whilst we previously emphasized the abundance of reworked clasts (fragmental and impact-melt breccia clasts), this is an imperfect criterion: one howardite with abundant re-worked clasts (EET 99408) shows no evidence of solar wind Ne (SW-Ne), yet, two of our alleged fragmental howardites have clear SW-Ne signatures (LEW 85313, MET 00423) [7, 8]. We are now investigating the diversity in minor and trace element contents of low-Ca pyroxene clasts in howardites as a measure of regolith grade, and will begin analyses of such grains within reworked clasts. Our hypothesis is that regolithic howardites (and the breccia clasts they contain) will show greater diversity because they sampled more diverse diogenitic plutons than fragmental howardites, which formed from ejecta from only a few impacts [e.g. 4]. Our initial LA-ICP-MS work showed ranges in trace element diversity in low-Ca pyroxenes (estimated from the standard error of the mean of analyses), where those howardites considered of medium to high regolithic grade showed greater diversity [9]. Our EMPA results (from a larger howardite suite) show an overall greater diversity in our putative medium to high regolithic grade howardites, though there are exceptions. The greatest diversity is found for paired howardites GRO 95574 and GRO 95581, which were not considered regolithic in our initial study. We will continue investigating avenues to determine regolith maturity in thin section, factoring in bulk rock compositional data, and will coordinate these studies with noble gas results.

Barium isotope abundances in meteorites and their implications for early Solar System evolution

NASA Astrophysics Data System (ADS)

Bermingham, K. R.; Mezger, K.; Scherer, E. E.; Horan, M. F.; Carlson, R. W.; Upadhyay, D.; Magna, T.; Pack, A.

2016-02-01

Several nucleosynthetic processes contributed material to the Solar System, but the relative contributions of each process, the timing of their input into the solar nebula, and how well these components were homogenized in the solar nebula remain only partially constrained. The Ba isotope system is particularly useful in addressing these issues because Ba isotopes are synthesized via three nucleosynthetic processes (s-, r-, p-process). In this study, high precision Ba isotope analyses of 22 different whole rock chondrites and achondrites (carbonaceous chondrites, ordinary chondrites, enstatite chondrites, Martian meteorites, and eucrites) were performed to constrain the distribution of Ba isotopes on the regional scale in the Solar System. A melting method using aerodynamic levitation and CO2-laser heating was used to oxidize SiC, a primary carrier of Ba among presolar grains in carbonaceous chondrites. Destruction of these grains during the fusion process enabled the complete digestion of these samples. The Ba isotope data presented here are thus the first for which complete dissolution of the bulk meteorite samples was certain. Enstatite chondrites, ordinary chondrites, and all achondrites measured here possess Ba isotope compositions that are not resolved from the terrestrial composition. Barium isotope anomalies are evident in most of the carbonaceous chondrites analyzed, but the 135Ba anomalies are generally smaller than previously reported for similarly sized splits of CM2 meteorites. Variation in the size of the 135Ba anomaly is also apparent in fused samples from the same parent body (e.g., CM2 meteorites) and in different pieces from the same meteorite (e.g., Orgueil, CI). Here, we investigate the potential causes of variability in 135Ba, including the contribution of radiogenic 135Ba from the decay of 135Cs and incomplete homogenization of the presolar components on the <0.8 g sample scale.

Chemical composition of Mars

USGS Publications Warehouse

Morgan, J.W.; Anders, E.

1979-01-01

The composition of Mars has been calculated from the cosmochemical model of Ganapathy and Anders (1974) which assumes that planets and chondrites underwent the same 4 fractionation processes in the solar nebula. Because elements of similar volatility stay together in these processes, only 4 index elements (U, Fe, K and Tl or Ar36) are needed to calculate the abundances of all 83 elements in the planet. The values chosen are U = 28 ppb, K = 62 ppm (based on K U = 2200 from orbital ??-spectrometry and on thermal history calculations by Tokso??z and Hsui (1978) Fe = 26.72% (from geophysical data), and Tl = 0.14 ppb (from the Ar36 and Ar40 abundances measured by Viking). The mantle of Mars is an iron-rich [Mg/(Mg + Fe) = 0.77] garnet wehrlite (?? = 3.52-3.54 g/cm3), similar to McGetchin and Smyth's (1978) estimate but containing more Ca and Al. It is nearly identical to the bulk Moon composition of Morgan et al. (1978b). The core makes up 0.19 of the planet and contains 3.5% S-much less than estimated by other models. Volatiles have nearly Moon-like abundances, being depleted relative to the Earth by factors of 0.36 (K-group, Tcond = 600-1300 K) or 0.029 (Tl group, Tcond < 600 K). The water abundance corresponds to a 9 m layer, but could be higher by as much as a factor of 11. Comparison of model compositions for 5 differentiated planets (Earth, Venus, Mars, Moon, and eucrite parent body) suggests that volatile depletion correlates mainly with size rather than with radial distance from the Sun. However, the relatively high volatile content of shergottites and some chondrites shows that the correlation is not simple; other factors must also be involved. ?? 1979.

Evaporative fractionation of volatile stable isotopes and their bearing on the origin of the Moon

PubMed Central

Day, James M. D.; Moynier, Frederic

2014-01-01

The Moon is depleted in volatile elements relative to the Earth and Mars. Low abundances of volatile elements, fractionated stable isotope ratios of S, Cl, K and Zn, high μ (238U/204Pb) and long-term Rb/Sr depletion are distinguishing features of the Moon, relative to the Earth. These geochemical characteristics indicate both inheritance of volatile-depleted materials that formed the Moon and planets and subsequent evaporative loss of volatile elements that occurred during lunar formation and differentiation. Models of volatile loss through localized eruptive degassing are not consistent with the available S, Cl, Zn and K isotopes and abundance data for the Moon. The most probable cause of volatile depletion is global-scale evaporation resulting from a giant impact or a magma ocean phase where inefficient volatile loss during magmatic convection led to the present distribution of volatile elements within mantle and crustal reservoirs. Problems exist for models of planetary volatile depletion following giant impact. Most critically, in this model, the volatile loss requires preferential delivery and retention of late-accreted volatiles to the Earth compared with the Moon. Different proportions of late-accreted mass are computed to explain present-day distributions of volatile and moderately volatile elements (e.g. Pb, Zn; 5 to >10%) relative to highly siderophile elements (approx. 0.5%) for the Earth. Models of early magma ocean phases may be more effective in explaining the volatile loss. Basaltic materials (e.g. eucrites and angrites) from highly differentiated airless asteroids are volatile-depleted, like the Moon, whereas the Earth and Mars have proportionally greater volatile contents. Parent-body size and the existence of early atmospheres are therefore likely to represent fundamental controls on planetary volatile retention or loss. PMID:25114311

Euhedral metallic-Fe-Ni grains in extraterrestrial samples

NASA Technical Reports Server (NTRS)

Rubin, Alan E.

1993-01-01

Metallic Fe-Ni is rare in terrestrial rocks, being largely restricted to serpentinized peridotites and volcanic rocks that assimilated carbonaceous material. In contrast, metallic Fe-Ni is nearly ubiquitous among extraterrestrial samples (i.e., meteorites, lunar rocks, and interplanetary dust particles). Anhedral grains are common. For example, in eucrites and lunar basalts, most of the metallic Fe-Ni occurs interstitially between silicate grains and thus tends to have irregular morphologies. In many porphyritic chondrules, metallic Fe-Ni and troilite form rounded blebs in the mesostasis because their precursors were immiscible droplets. In metamorphosed ordinary chondrites, metallic Fe-Ni and troilite form coarse anhedral grains. Some of the metallic Fe-Ni and troilite grains has also been mobilized and injected into fractures in adjacent silicate grains where local shock-reheating temperatures reached the Fe-FeS eutectic (988 C). In interplanetary dust particles metallic Fe-Ni most commonly occurs along with sulfide as spheroids and fragments. Euhedral metallic Fe-Ni grains are extremely rare. Several conditions must be met before such grains can form: (1) grain growth must occur at free surfaces, restricting euhedral metallic Fe-Ni grains to systems that are igneous or undergoing vapor-deposition; (2) the metal (+/-) sulfide assemblage must have an appropriate bulk composition so that taenite is the liquidus phase in igneous systems or the stable condensate phase in vapor-deposition systems; and (3) metallic Fe-Ni grains must remain underformed during subsequent compaction, thermal metamorphism, and shock. Because of these restrictions, the occurrence of euhedral metallic Fe-Ni grains in an object can potentially provide important petrogenetic information. Despite its rarity, euhedral metallic Fe-Ni occurs in a wide variety of extraterrestrial materials. Some of these materials formed in the solar nebula; others formed on parent body surfaces by meteoroid impacts.

Parental perceptions of children's body shapes.

PubMed

Zalilah, M S; Anida, H A; Merlin, Ang

2003-12-01

The aim was to determine the differences in parents' perceptions of boys' and girls' body shapes and the explanations for the emphasis on body shape care of children. Subjects were low-income parents (n = 158) of preschoolers attending preschools in Kuala Lumpur, Malaysia. Parental perceptions of children's body shapes were assessed based on their rankings (scale of 1 to 7) of four attributes (ideal, healthy, fat and thin) for boy and girl figures. Parental responses to five questions on the importance of body shape were also obtained. Parental rankings of ideal and healthy body shapes were significantly lower for girls than boys (p < 0.001). However, mothers' and fathers' rankings of boys' and girls' body shapes were not significantly different. for both boys and girls, parental ratings for ideal body shape were significantly lower than for healthy body shape (p < 0.001). The majority of parents indicated that children's body shape is important for their future health, self enhancement, social interaction and career. With the increasing prevalence of body dissatisfaction among Malaysian children, these findings contribute to the understanding of parental roles in the development of body image and perhaps, in the etiology of body dissatisfaction among children.

Meteoritical Implications of the Vesta Asteroid Family

NASA Astrophysics Data System (ADS)

Bell, J. F.

1993-07-01

The discovery of a large dynamical family of basaltic asteroids associated with Vesta and extending to the 3:1 Jupiter resonance [1] provides firm evidence at last that Vesta is the actual parent body of the basaltic achondrite meteorites [2]. This discovery raises several interesting questions. The Vesta family demonstrates that objects as large as ~10km can be ejected from large asteroids at velocities up to 500 m/sec, which is adequate to deliver material to a strong resonance from almost anywhere in the asteroid belt. However, most other asteroid families show a much smaller range of ejection velocities and a more symmetrical distribution of the fragments in orbital element space. These families probably come from complete disruption of parent bodies, which would therefore appear to be the dominant process. Meteoritical evidence is also relevant. There are at least six large dunite (A-class) asteroids, only one of which is providing brachinites to the Earth. Even more striking, the Nysa asteroid family is predominantly composed of the mysterious F-class asteroids, which have no meteorite analog at all. The evidence suggests that the Vesta event is atypical and that there is considerable bias in meteorite delivery. The family is extended in a but narrowly confined in e and i. Curiously, Vesta is not at one end but in the middle. The very narrow sunward leg of the family contains a rare pure-olivine (Class A) asteroid among the many eucrites (Class V) and diogenites (Class J), while in the more diffuse anti-sunward leg no olivine objects have yet been found. This mineral distribution mimics the mineral map of Vesta derived from telescopic spectroscopy [3], in which a small olivine spot is semi-antipodal to a large diogenite patch. This suggests that the sunward leg is direct ejecta from a large crater, while the anti-sunward leg (and the populartion of HEDs reaching Earth) is composed of crustal fragments spalled off by focused shock waves. This mechanism is well-known from lab experiments [4] and probably causes the jumbled terrain antipodal to impact basins on the Moon and Mercury. Finally, it is now clear that the association between the HED clan and the pallasites is coincidental. We may expect many more such false genetic links between meteorite classes as more oxygen isotope data is obtained. References: [1] Binzel R. P. and Xu S. (1993) Science, 260, 186- 191. [2] Gaffey M. J. (1993) Science, 260, 167-168. [3] Gaffey M. J. (1983) LPS XIV, 231-232. [4] Horz F. and Schaal R. B. (1981) Icarus, 46, 337-353.

Space Weathering on 4 Vesta: Processes and Products

NASA Technical Reports Server (NTRS)

Pieters, C. M.; Blewett, D. T.; Gaffey, M.; Mittlefehldt, D. W.; De Sanctis, M. C.; Reddy, V.; Nathues, A.; Denevi, B. W.; Li, J. Y.; McCord, T. B.;

Accuracy of self- and parental perception of overweight among Latino preadolescents.

PubMed

Intagliata, Valentina; Ip, Edward H; Gesell, Sabina B; Barkin, Shari L

2008-01-01

This investigation examines self-perception and parental perception of child body size and factors associated with accurate parental perception of child body size. Latino at-risk for overweight (AROW) and/or overweight preadolescent children (ages 8-11 years) along with their parents were recruited (N=123 dyads). Children's body mass index (BMI) was measured but not discussed before participants were shown pictures of body sizes and asked to select the image that represented the child's body. The correlation between the child's body size selection and the child's actual BMI was 0.117 (p=0.20) whereas the correlation between the parent's assessment of the child's body size and the child's actual BMI was 0.470 (p<0.001). Logistic regression revealed that only parental education level (> or =college) was associated with a more accurate parental perception of their child's body size (OR: 0.11/95% CI: 0.01, 0.89) while child's sex, parental BMI, and parental health status were not associated with a perception that corresponded to the child's BMI. The sample was drawn from a single community clinic in Forsyth County which serves a large population of newer Latino immigrants in the county. The results indicate that (1) Latino AROW/overweight preadolescent children do not have an accurate perception of their own body size; (2) Latino parents have a more accurate perception of their child's body size with a moderately sized correlation suggesting that their perception of their child's body size is frequently inaccurate; and (3) Latino parents with higher education perceive their child's body size more accurately than less educated parents.

Magnetic fields on asteroid 4 Vesta recorded by the Millbillillie eucrite

NASA Astrophysics Data System (ADS)

Weiss, B. P.; Fu, R.

2011-12-01

The detection of past dynamo activity on the asteroid 4 Vesta would confirm the existence of a metallic core, placing important constraints on its accretional and thermal history. Knowledge of the strength and duration of a dynamo on 4 Vesta also has important implications for the theoretical understanding of dynamo generation in small bodies. Magnetic fields from a putative core dynamo may have been recorded as remanent magnetization in achondritic meteorites of the howardite-eucrite-diogenite (HED) clan, which are thought to originate from the asteroid. To search for evidence for past dynamo activity, we performed a paleomagnetic study of nine mutually oriented samples of the Millbillillie eucrite. We found that the magnitude and direction of the magnetization change systematically for samples progressively farther away from the fusion crust, indicating that the samples were not remagnetized on Earth and that the interior samples carry an extraterrestrial magnetization. The fusion crust is ~1000 times more magnetic per unit mass than the interior, which was likely a source of contamination in earlier studies of bulk samples from this meteorite. Two interior samples were subjected to alternating field (AF) demagnetization up to 290 mT. We found a high coercivity (HC) component of magnetization carried by grains with coercivities between 70 and 180 mT. The HC magnetization is approximately unidirectional in the subsamples. The AF demagnetization profile of this component is similar to that of an anhysteretic remanent magnetization (ARM), suggesting that it may represent a thermoremanent magnetization (TRM). Under this assumption, our ARM paleointensity experiments yield field strengths of 2-3 μT while our IRM paleointensities are between 5 and 8 μT. Ongoing analysis of additional samples will further test this result. The HC magnetization may record 1) transient impact-generated fields, 2) remanent crustal fields, or 3) dynamo fields. Case 1) is unlikely if the sample has a thermoremanence because stable magnetization over the wide coercivity range observed for the HC component requires a magnetic field stable for the duration of the cooling process. Furthermore, the characteristic coercivities of the HC magnetization are very high compared to typical values for shock remanent magnetization. In case 2), the strength of putative impact-generated crustal fields on the moon suggests that impacts on Vesta would have caused remanent crustal fields of < 2 μT strength, which is below our observed paleointensities. Remanent crustal fields stronger than ~2 μT require a different magnetizing source, such as an earlier dynamo. Together, these facts suggest that the HC magnetization is unlikely to be a result of meteoroid bombardment and more probably record dynamo fields or remanent crustal fields due to an earlier dynamo. We therefore regard our results as tentative evidence of a past dynamo on 4 Vesta

Core Formation on Asteroid 4 Vesta: Iron Rain in a Silicate Magma Ocean

NASA Astrophysics Data System (ADS)

Kiefer, W. S.; Mittlefehldt, D. W.

2017-07-01

Initially small liquid metal drops must grow to about 10 cm in size before sinking through the convecting silicate magma ocean to form a core. The required magma temperature is consistent with moderately siderophile element abundances in eucrites.

Howardite Noble Gases as Indicators of Asteroid Surface Processing

NASA Technical Reports Server (NTRS)

Cartwright, J. A.; Mittlefehldt, D. W.; Herrin, J. S.; Ott, U.

2011-01-01

The HED (Howardite, Eucrite and Diogenite) group meteorites likely or iginate from the Asteroid 4 Vesta - one of two asteroid targets of NA SA's Dawn mission. Whilst Howardites are polymict breccias of eucriti c and diogenitic material that often contain "regolithic" petrologica l features, neither their exact regolithic nature nor their formation processes are well defined. As the Solar Wind (SW) noble gas compon ent is implanted onto surfaces of solar system bodies, noble gas anal yses of Howardites provides a key indicator of regolithic origin. In addition to SW, previous work by suggested that restricted Ni (300-12 00 micro g/g) and Al2O3 (8-9 wt%) contents may indicate an ancient we ll-mixed regolith. Our research combines petrological, compositional and noble gas analyses to help improve understanding of asteroid reg olith formation processes, which will play an intergral part in the i nterpretation of Dawn mission data. Following compositional and petrological analyses, we developed a regolith grading scheme for our sampl e set of 30 Howardites and polymict Eucrites. In order to test the r egolith indicators suggested by, our 8 selected samples exhibited a r ange of Ni, Al2O3 contents and regolithic grades. Noble gas analyses were performed using furnace stepheating on our MAP 215-50 noble gas mass spectrometer. Of our 8 howardites, only 3 showed evidence of SW noble gases (e.g approaching Ne-20/Ne-22 approximately equals 13.75, Ne-21/Ne-22 approximately equals 0.033). As these samples display low regolithic grades and a range of Ni and Al2O3 contents, so far we are unable to find any correlation between these indicators and "regolit hic" origin. These results have a number of implications for both Ho wardite and Vesta formation, and may suggest complex surface stratigr aphies and surface-gardening processes.

Partial melting of the St. Severin (LL) and Lost City (H) ordinary chondrites: One step backwards and two steps forward

NASA Technical Reports Server (NTRS)

Jurewicz, A. J. G.; Jones, J. H.; Mittlefehldt, D. W.

1994-01-01

This study looks at partial melting in H and LL chondrites at nearly one atmosphere of total pressure as part of a continuing study of the origins of basaltic achondrites. Previously, melting experiments on anhydrous CM and CV chondrites showed that, near its solidus, the CM chondrite produced melts having major element chemistries similar to the Sioux County eucrite; but, the pyroxenes in the residuum were too iron-rich to form diogenites. Our preliminary results from melting experiments on ordinary (H, LL) chondrites suggested that, although the melts did not look like any known eucrites, pyroxenes from these charges bracketed the compositional range of pyroxenes found in diogenites. We had used the Fe/Mg exchange coefficients calculated for olivine, pyroxene, and melt in these charges to evaluate the approach to equilibrium, which appeared to be excellent. Unfortunately, mass balance calculations later indicated to us that, unlike our CM and CV charges, the LL and H experimental charges had lost significant amounts of iron to their (Pt or PtRh) supports. Apparently, pyroxene stability in chondritic systems is quite sensitive to the amount of FeO, and it was this unrecognized change in the bulk iron content which had stabilized the high temperature, highly magnesian pyroxenes. Accordingly, this work reinvestigates the phase equilibria of ordinary chondrites, eliminating iron and nickel loss, and reports significant differences. It also looks closely at how the iron and sodium in the bulk charge affect the stability of pyroxene, and it comments on how these new results apply to the problems of diogenite and eucrite petrogenesis.

The longitudinal causal directionality between body image distress and self-esteem among Korean adolescents: the moderating effect of relationships with parents.

PubMed

Park, Woochul; Epstein, Norman B

2013-04-01

This study examined the longitudinal relationship between self-esteem and body image distress, as well as the moderating effect of relationships with parents, among adolescents in Korea, using nationally representative prospective panel data. Regarding causal direction, the findings supported bi-directionality for girls, but for boys the association was unidirectional, in that their self-esteem predicted body image distress, but not vice versa. A gender difference also emerged in the moderating effect of quality of relationships with parents. For girls, relationships with parents moderated the effect of body image distress on self-esteem, such that when relationships with parents were better, the effect of greater body image distress on subsequent lower self-esteem was stronger than when relationships with parents were less positive. For boys, relationships with parents moderated the influence of self-esteem on body image distress, such that self-esteem reduced body image distress more when boys had better relationships with parents. Copyright © 2013. Published by Elsevier Ltd.

Body image perceptions in Western and post-communist countries: a cross-cultural pilot study of children and parents.

PubMed

Humenikova, Lenka; Gates, Gail E

2008-07-01

The development of an unrealistic ideal body image and body size dissatisfaction among children is common in Western countries, including the USA and many European nations. However, little is known about children's body image perceptions in post-communist countries. This pilot study evaluated body image perceptions in a sample of Czech school-aged children and their parents and compared them with the perceptions of American children and parents. Ninety-seven Czech and 45 American 4th-6th graders and their parents from eight urban schools participated in this study. A previously developed silhouette body image instrument was utilized in a parent questionnaire and during child interviews to measure perceived and ideal body image perceptions of children and parents. Descriptive statistics, independent t-tests and paired t-tests were used to compare differences between children's and parents' perceived and ideal body image perceptions. Associations between body image perceptions and other variables were explored using bivariate correlations. American children had a thinner ideal body image compared with Czech children (P < 0.05). However, a larger proportion of Czech boys desired to be thinner compared with American boys (34.2% vs. 20%). Parent's ideal body image for their children did not differ by nationality (P = 0.858). While the pressure on children to look thinner was apparent among both American and Czech children, Czech children considered a larger body size as more ideal. A future study should evaluate body image perceptions and factors influencing these perceptions in a representative sample of Czech children and parents.

Spectroscopic Characterization of Mineralogy Across Vesta: Evidence of Different Lithologies

NASA Technical Reports Server (NTRS)

De Sanotis, M. C.; Ammannito, E.; Filacchione, G.; Capria, M. T.; Tosi, F.; Capaccioni, F.; Zambon, F.; Carraro, F.; Fonte, S.; Frigeri, A.;

[Impact on the development of parental awareness of excess weight in children].

PubMed

Łupińska, Anna; Chlebna-Sokół, Danuta

2015-04-01

A lot of publications emphasize the special role of parents' eating habits and their lifestyle on the prevalence of excess body weight in children. The aim of this study was to answer the question whether parents of children who are overweight and obese are aware of this problem and what factors affect their perception of the excess body weight degree in their offspring. The study included 137 children aged 6,5- 13,5 years. 23 respondents were overweight and 76 obese. Compared group consisted of 113 children. All patients underwent physical examination with anthropometric measurements. Parents were asked to complete a questionnaire, where they evaluated the degree of excess body weight of their child. We also asked about both parents' weight and body height, their education and chronic diseases occurring in the family. In the group of obese children 56.2% of the respondents came from families where one parent had excess body weight while 32.9% of them from families where this problem affected both parents. In 51.3% of patients with a body mass index (BMI) above 95 centil, parents wrongly assessed the degree of excess body weight of their child, in overweight group this proportion accounted for 8.7%. There was a statistically significant (p = 0.007) correlation between the degree of children's excess body weight and the ability of parents to estimate that. Parents' education had no influence on the incidence of excess body weight in children and their ability to determine its extent. In the group of obese and overweight children only 4% of parents recognized obesity as a chronic disease. Parents of children who are overweight and obese have lower awareness about their child's weight in comparison to parents of children with normal weight. There is a statistical correlation between parents' perception of excess body weight and the development of obesity in children. © 2015 MEDPRESS.

Development and validation of parenting measures for body image and eating patterns in childhood.

PubMed

Damiano, Stephanie R; Hart, Laura M; Paxton, Susan J

2015-01-01

Evidence-based parenting interventions are important in assisting parents to help their children develop healthy body image and eating patterns. To adequately assess the impact of parenting interventions, valid parent measures are required. The aim of this study was to develop and assess the validity and reliability of two new parent measures, the Parenting Intentions for Body image and Eating patterns in Childhood (Parenting Intentions BEC) and the Knowledge Test for Body image and Eating patterns in Childhood (Knowledge Test BEC). Participants were 27 professionals working in research or clinical treatment of body dissatisfaction or eating disorders, and 75 parents of children aged 2-6 years, who completed the measures via an online questionnaire. Seven scenarios were developed for the Parenting Intentions BEC to describe common experiences about the body and food that parents might need to respond to in front of their child. Parents ranked four behavioural intentions, derived from the current literature on parenting risk factors for body dissatisfaction and unhealthy eating patterns in children. Two subscales were created, one representing positive behavioural intentions, the other negative behavioural intentions. After piloting a larger pool of items, 13 statements were used to construct the Knowledge Test BEC. These were designed to be factual statements about the influence of parent language, media, family meals, healthy eating, and self-esteem on child eating and body image. The validity of both measures was tested by comparing parent and professional scores, and reliability was assessed by comparing parent scores over two testing occasions. Compared with parents, professionals reported significantly higher scores on the Positive Intentions subscale and significantly lower on the Negative Intentions subscale of the Parenting Intentions BEC; confirming the discriminant validity of six out of the seven scenarios. Test-retest reliability was also confirmed as parent scores on the two Parenting Intentions subscales did not differ over time. Eleven out of the 13 Knowledge Test items demonstrated sufficient discriminant validity and test-retest reliability. Overall, results indicated that the six-scenario Parenting Intentions BEC and the 11-item Knowledge Test BEC are valid and reliable measures for parents of young children.

Long-lived magnetism on chondrite parent bodies

NASA Astrophysics Data System (ADS)

Shah, Jay; Bates, Helena C.; Muxworthy, Adrian R.; Hezel, Dominik C.; Russell, Sara S.; Genge, Matthew J.

2017-10-01

We present evidence for both early- and late-stage magnetic activity on the CV and L/LL parent bodies respectively from chondrules in Vigarano and Bjurböle. Using micro-CT scans to re-orientate chondrules to their in-situ positions, we present a new micron-scale protocol for the paleomagnetic conglomerate test. The paleomagnetic conglomerate test determines at 95% confidence, whether clasts within a conglomerate were magnetized before or after agglomeration, i.e., for a chondritic meteorite whether the chondrules carry a pre- or post-accretionary remanent magnetization. We found both meteorites passed the conglomerate test, i.e., the chondrules had randomly orientated magnetizations. Vigarano's heterogeneous magnetization is likely of shock origin, due to the 10 to 20 GPa impacts that brecciated its precursor material on the parent body and transported it to re-accrete as the Vigarano breccia. The magnetization was likely acquired during the break-up of the original body, indicating a CV parent body dynamo was active ∼9 Ma after Solar System formation. Bjurböle's magnetization is due to tetrataenite, which transformed from taenite as the parent body cooled to below 320 °C, when an ambient magnetic field imparted a remanence. We argue either the high intrinsic anisotropy of tetrataenite or brecciation on the parent body manifests as a randomly orientated distribution, and a L/LL parent body dynamo must have been active at least 80 to 140 Ma after peak metamorphism. Primitive chondrites did not originate from entirely primitive, never molten and/or differentiated parent bodies. Primitive chondrite parent bodies consisted of a differentiated interior sustaining a long-lived magnetic dynamo, encrusted by a layer of incrementally accreted primitive meteoritic material. The different ages of carbonaceous and ordinary chondrite parent bodies might indicate a general difference between carbonaceous and ordinary chondrite parent bodies, and/or formation location in the protoplanetary disk.

Small-scale impacts as potential trigger for landslides on small Solar system bodies

NASA Astrophysics Data System (ADS)

Hofmann, Marc; Sierks, Holger; Blum, Jürgen

2017-07-01

We conducted a set of experiments to investigate whether millimetre-sized impactors impinging on a granular material at several m s-1 are able to trigger avalanches on small, atmosphereless planetary bodies. These experiments were carried out at the Zentrum für angewandte Raumfahrttechnologie und Mikrogravitation (ZARM) drop tower facility in Bremen, Germany to facilitate a reduced gravity environment. Additional data were gathered at Earth gravity levels in the laboratory. As sample materials we used a ground Howardites, Eucrites and Diogenites (HED) meteorite and the Johnson Space Center (JSC) Mars-1 Martian soil simulant. We found that this type of small-scale impact can trigger avalanches with a moderate probability, if the target material is tilted to an angle close to the angle of repose. We additionally simulated a small-scale impact using the discrete element method code esys-particle. These simulations show that energy transfer from impactor to the target material is most efficient at low- and moderate-impactor inclinations and the transferred energy is retained in particles close to the surface due to a rapid dissipation of energy in lower material layers driven by inelastic collisions. Through Monte Carlo simulations we estimate the time-scale on which small-scale impacts with the observed characteristics will trigger avalanches covering all steep slopes on the surface of a small planetary body to be of the order 105 yr.

Reevaluating Surface Composition of Asteroid (4) Vesta by Comparing HED Spectral Data with Dawn Framing Camera (FC) Observations

NASA Astrophysics Data System (ADS)

Giebner, T.; Jaumann, R.; Schröder, S.

2016-08-01

This master's thesis project tries to reevaluate previous findings on asteroid (4) Vesta's surface composition by using DAWN FC Filter image ratios in a new way in order to identify HED (howardite, eucrite, diogenite) lithologies on the surface.

Parent-Child Discrepancy on Children's Body Weight Perception: The Role of Attachment Security.

PubMed

Uccula, Arcangelo; Nuvoli, Gianfranco

2017-01-01

The discrepancies between parents and their children on the description of the behavior and representations of their children have been shown in various studies. Other researchers have reported the parents' difficulty in correctly identifying the weight status of their children. The purpose of our study was to investigate the parent's attributional accuracy on their children's body weight perception in relation to the children attachment security. It was hypothesized that insecure children's parents have a greater discrepancy with their children compared to secure children with their parents. The research participants were 217 children, aged between 5 and 11 years of both genders, and their parents. The attachment pattern was measured by the SAT of Klagsbrun and Bowlby, with the Italian version of Attili. The children were also shown a set of figure body-drawings with which to measure the perception of their weight status. Parents answered a questionnaire to find out the parental attribution of their children's perception. The results show that the body weight perception of insecure children's parents have a greater discrepancy with their children's body weight perception compared with parentally secure children. In particular, parents of insecure children tend to underestimate the perception of their children. This result is most evident in disorganized children. In addition, the perception of insecure children's parents show a greater correlation with children's actual weight rather than with their children's perception. These results suggest that the discrepancies on the perception of children's body weight between parents and children may be influenced by the poor parental attunement to their children's internal states, which characterizes the insecure parent-child attachment relationship.

Parents' concern about their children's weight.

PubMed

Lampard, Amy M; Byrne, Susan M; Zubrick, Stephen R; Davis, Elizabeth A

2008-01-01

Firstly, to investigate the degree of concern parents feel about their children's weight (parental concern). Secondly, to identify factors that influence this concern, and to test a model of parental concern using structural equation modeling. A total of 347 non-overweight, overweight, and obese children (aged 6-13; Mean = 9.5, SD = 1.8) and their parents. Children and their parents attended an assessment session during which they were weighed and measured. Parents were administered a structured interview, which included the Eating Disorder Examination, and completed the Pediatric Quality of Life Inventory (parent proxy), and the Children's Body Image Scale. Eighty-two percent of parents of overweight children, and 18% of parents of obese children reported little parental concern. Higher parental concern was associated with higher child Body Mass Index, less parental underestimation of child body size, and lower child health-related quality of life. Interventions targeting childhood obesity should aim to optimise parental concern by reducing parents' underestimation of child body size and increasing their awareness of the effects of overweight and obesity on children's health and quality of life.

Relationship of Blood Cholesterol to Body Composition, Physical Fitness, and Dietary Intake Measures in Third-Grade Children and Their Parents.

ERIC Educational Resources Information Center

Hopper, Chris A.; Gruber, Mary B.; Munoz, Kathy D.; MacConnie, Susan E.; Pfingston, Yvonne M.; Nguyen, Kim

2001-01-01

Investigated interrelationships between blood cholesterol levels, body composition, diet, and physical fitness among third graders and their parents. Data from blood and body measurements, children's physical fitness tests, parents' physical activity surveys, and children's and parents' dietary recalls highlighted significant mild-to-moderate…

Multiple parent bodies of ordinary chondrites

NASA Technical Reports Server (NTRS)

Yomogida, K.; Matsui, T.

1984-01-01

Thermal histories of chondrite parent bodies are calculated from an initial state with material in a powder-like form, taking into account the effect of consolidation state on thermal conductivity. The very low thermal conductivity of the starting materials makes it possible for a small body with a radius of less than 100 km to be heated by several hundred degrees even if long-lived radioactive elements in chondritic abundances are the only source of heat. The maximum temperature is determined primarily by the temperature at which sintering of the constituent materials occurs. The thermal state of the interior of a chondrite parent body after sintering has begun is nearly isothermal. Near the surface, however, where the material is unconsolidated and the thermal conductivity is much lower, the thermal gradient is quite large. This result contradicts the conventional 'onion-shell' model of chondrite parent bodies. But because the internal temperature is almost constant through the whole body, it supports a 'multiple-parent bodies' model, according to which each petrologic type of chondrite comes from a different parent body.

Nature and evolution of the meteorite parent bodies: Evidence from petrology and metallurgy

NASA Technical Reports Server (NTRS)

Wood, J. A.

1978-01-01

The physical as well as chemical properties of the meteorite parent bodies are reviewed and it is concluded that many differentiated meteorites were likely formed in asteroidal-sized parents. A new model is developed for the formation of pallasites at the interface between an iron core and olivine mantle in differentiated bodies only about 10 km in diameter, which are later incorporated into a second generation of larger (100 km) parent bodies.

Unambiguous Spectral Evidence for High- (and Low-) Calcium Pyroxene in Asteroids and Meteorites

NASA Technical Reports Server (NTRS)

Sunshine, J. M.; Bus, S. J.; Burbine, T. H.; McCoy, T. J.; Binzel, R. P.

2002-01-01

Several new S-asteroid spectra are modeled and found to contain both low- and high-calcium pyroxenes. Similar results are obtained for spectra of eucrites. Their inferred mineralogy is very consistent with petrographic results, lending confidence to the asteroid analyses. Additional information is contained in the original extended abstract.

The lunar interior

NASA Technical Reports Server (NTRS)

Anderson, D. L.; Kovach, R. L.

1972-01-01

The compressional velocities are estimated for materials in the lunar interior and compared with lunar seismic results. The lower crust has velocities appropriate for basalts or anorthosites. The high velocities associated with the uppermost mantle imply high densities and a change in composition to a lighter assemblage at depths of the order of 120 km. Calcium and aluminum are probably important components of the upper mantle and are deficient in the lower mantle. Much of the moon may have accreted from material similar in composition to eucrites. The important mineral of the upper mantle is garnet; possible accessory minerals are kyanite, spinel, and rutile. If the seismic results stand up, the high velocity layer in the moon is more likely to be a high pressure form of anorthosite than eclogite, pyroxenite, or dunite. The thickness of the layer is of the order of 50 km. Cosmic abundances can be maintained if the lower mantle is ferromagnesium silicate with minimal amounts of calcium and aluminum. Achondrites such as eucrites and howardites have more of the required characteristics of the lunar interior than carbonaceous chondrites. A density inversion in the moon is a strong possibility.

The production rate of cosmogenic 21-Ne in chondrites deduced from 81-Kr measurements

NASA Technical Reports Server (NTRS)

Schultz, L.; Freundel, M.

1986-01-01

Cosmogenic Ne-21 is used widely to calculate exposure ages of stone meteorites. In order to do so, the production rate P(21) must be known. This rate, however, is dependent on the chemical composition of the meteorite as well as the mass of, and position within, the meteoroid during its exposure to the cosmic radiation. Even for a mean shielding the production rates determined from measurments of different radionuclides vary by a factor of two. A method that can be used to determine exposure ages of meteorites that avoids shielding and chemical composition corrections is the -81-Kr-Kr-method. However, for chondrites, in many cases, the direct determination of production rates for the Kr isotopes is prevented by the trapped gases and the neutron effects on bromine. Therefore, this method was applied to four eucrite falls and then their 81-Kr-83-Kr-ages were compared to their cosmogenic Ne-21 and Ar-38 concentrations. The eucrites Bouvante-le-Haut, Juvinas, Sioux County, and Stannern were chosen for these measurements because of their similar chemical composition regarding the major elements.

Effect of the Parent-Adolescent Relationship on Adolescent Boys' Body Image and Subjective Well-Being.

PubMed

Walter, Ofra; Shenaar-Golan, Vered

2017-07-01

Adolescent boys must cope with physical changes that hamper their ability to form a positive body image. Sociocultural messages influence the concepts of body image, personal appearance, and weight, encouraging men to develop lean and muscular bodies. The current study examined adolescent boys' body image and its relationship to their subjective well-being (SWB) and the effect of the parent-adolescent relationship on body image and SWB. Participating in the research were 107 adolescent boys in Israel, aged 13 to 18 years. Four questionnaires were utilized: demographic, body mass index, Body Investment Scale, and Personal Well-Being Index. The findings indicate a significant, medium positive correlation between SWB and body image. After controlling for the variable of parent-adolescent relationship, the correlation weakened, indicating that the parent-adolescent relationship has no effect on adolescent boys' SWB and body image. Body image was reported to be a predictor of SWB.

School-Based BMI and Body Composition Screening and Parent Notification in California: Methods and Messages

ERIC Educational Resources Information Center

Madsen, Kristine A.; Linchey, Jennifer

2012-01-01

Background: School-based body mass index (BMI) or body composition screening is increasing, but little is known about the process of parent notification. Since 2001, California has required annual screening of body composition via the FITNESSGRAM, with optional notification. This study sought to identify the prevalence of parental notification…

Evaporative fractionation of volatile stable isotopes and their bearing on the origin of the Moon.

PubMed

Day, James M D; Moynier, Frederic

2014-09-13

The Moon is depleted in volatile elements relative to the Earth and Mars. Low abundances of volatile elements, fractionated stable isotope ratios of S, Cl, K and Zn, high μ ((238)U/(204)Pb) and long-term Rb/Sr depletion are distinguishing features of the Moon, relative to the Earth. These geochemical characteristics indicate both inheritance of volatile-depleted materials that formed the Moon and planets and subsequent evaporative loss of volatile elements that occurred during lunar formation and differentiation. Models of volatile loss through localized eruptive degassing are not consistent with the available S, Cl, Zn and K isotopes and abundance data for the Moon. The most probable cause of volatile depletion is global-scale evaporation resulting from a giant impact or a magma ocean phase where inefficient volatile loss during magmatic convection led to the present distribution of volatile elements within mantle and crustal reservoirs. Problems exist for models of planetary volatile depletion following giant impact. Most critically, in this model, the volatile loss requires preferential delivery and retention of late-accreted volatiles to the Earth compared with the Moon. Different proportions of late-accreted mass are computed to explain present-day distributions of volatile and moderately volatile elements (e.g. Pb, Zn; 5 to >10%) relative to highly siderophile elements (approx. 0.5%) for the Earth. Models of early magma ocean phases may be more effective in explaining the volatile loss. Basaltic materials (e.g. eucrites and angrites) from highly differentiated airless asteroids are volatile-depleted, like the Moon, whereas the Earth and Mars have proportionally greater volatile contents. Parent-body size and the existence of early atmospheres are therefore likely to represent fundamental controls on planetary volatile retention or loss. © 2014 The Author(s) Published by the Royal Society. All rights reserved.

Spectral measurements of howardites in support of the interpretation of the Dawn VIR spectra at Vesta

NASA Astrophysics Data System (ADS)

De Angelis, S.; Ammannito, E.; Di Iorio, T.; De Sanctis, M.; Mittlefehldt, D.

2014-07-01

The howardites, eucrites, and diogenites constitute a suite of meteorite lithologies (HED) known to be related to asteroid Vesta [1]. Howardites are physical mixtures of eucrites and diogenites. Howardites are divided in two subtypes: regolithic howardites are actually linked to the true regolith, while fragmental howardites are simple polymict breccias [2]. Mapping of Vesta's surface, as obtained with data from Visible and Infrared mapping Spectrometer (VIR) on Dawn [3,4], showed that it is mainly howarditic, with few regions of diogenite-rich and eucrite-rich terrains [5, 6]. In order to map quantitatively the distribution of lithologic types on Vesta, we are carrying on a study of a set of well-characterized howardites [7]. Spectra were measured on sample powders sieved to 75 μ m in the laboratories of the Istituto di Astrofisica e Planetologia Spaziali (IAPS-INAF) in Rome (Italy) and Brown University, in Providence (USA). Here we report about the measurements done at IAPS-INAF. The spectra of 33 samples have been acquired with the S.LAB setup, consisting in the FieldSpec Pro spectrometer (range 0.35-2.5 μ m, spatial resolution 0.5 cm^2) coupled with a goniometer (incidence i=30°, emission e=0°) [8]. Some representative spectra of the measured howardites are shown in the figure. The spectra are characterized by the two broad Fe^{2+} absorption bands near 1 and 2 μ m (BI and BII) indicative of pyroxenes. Band parameters relative to BI and BII have been calculated using the algorithm developed to process VIR spectra [4]. This enables us to compare laboratory data directly with the VIR results. Other weaker absorptions also characterize some spectra: the 0.5 μ m feature (Mn^{2+} or Cr^{3+}) and the 1.2 μ m feature possibly due to Fe^{2+} in plagioclases. The PRA04401 sample is characterized by a pyroxene-carbonaceous matter mixture [7].

School-based BMI and body composition screening and parent notification in California: methods and messages.

PubMed

Madsen, Kristine A; Linchey, Jennifer

2012-06-01

School-based body mass index (BMI) or body composition screening is increasing, but little is known about the process of parent notification. Since 2001, California has required annual screening of body composition via the FITNESSGRAM, with optional notification. This study sought to identify the prevalence of parental notification when screening is required but notification is optional, and the methods and messages used. Researchers conducted phone interviews with 851 school districts (89%) in California and reviewed notification materials from 54 districts. As of 2008, 53% of California districts notified parents of screening results. Many districts (24%) did not know the reason for their notification policy. Most districts notified parents via a letter mailed home (70%) or sent home with the child (18%). Whereas 79% of sample letters provided students' BMI, only 12% provided an explanation of BMI, and only half provided tips on what parents should do if concerned about their child's results. In California, where body composition screening is required but parent notification is not, approximately half of school districts elect to notify parents of results, most commonly via letter. Most letters do not explain BMI or percent body fat scores, nor do they suggest what parents should do for a child identified as at-risk. Further research to identify interpretable and actionable notification messages for parents will be critical if school-based BMI and body composition screening and notification is to reduce childhood obesity. Published 2012. This article is a U.S. Government work and is in the public domain in the USA.

Confident body, confident child: A randomized controlled trial evaluation of a parenting resource for promoting healthy body image and eating patterns in 2- to 6-year old children.

PubMed

Hart, Laura M; Damiano, Stephanie R; Paxton, Susan J

2016-05-01

Body image and eating patterns develop in early childhood and are influenced by the family environment. This research evaluated Confident Body, Confident Child (CBCC), an intervention for parents of 2- to 6-year-old children, designed to promote body satisfaction, healthy eating, and weight management in early childhood. A randomized controlled trial compared four groups: (A) received the CBCC resource pack and a workshop, (B) received the CBCC resource pack only, (C) received a nutrition-only resource and (D) received no interventions until all questionnaires were completed (i.e., functioned as waitlist control). Measures of parenting variables relevant to child body image and eating patterns, parent-report of child weight, and evaluation questions about the resource, were implemented pre- and post-intervention. At 6-weeks post-intervention, the CBCC resource was associated with significant reductions in parents' intentions to use behaviors that increase the risk of negative body attitudes or unhealthy eating in their children, in parents' use of feeding practices associated with childhood overweight, and in television watching during family meals. Significant increases in parents' intentions to use positive behaviors and knowledge of child body image and healthy eating patterns were also found. Superior results were found for the CBCC resource + workshop condition, suggesting it is the preferred delivery method. CBCC positively impacts parenting variables associated with childhood risk for body dissatisfaction, unhealthy eating and weight. © 2016 Wiley Periodicals, Inc. (Int J Eat Disord 2016; 49:458-472). © 2016 Wiley Periodicals, Inc.

A Model of Female Sexual Desire: Internalized Working Models of Parent-Child Relationships and Sexual Body Self-Representations.

PubMed

Cherkasskaya, Eugenia; Rosario, Margaret

2017-11-01

The etiology of low female sexual desire, the most prevalent sexual complaint in women, is multi-determined, implicating biological and psychological factors, including women's early parent-child relationships and bodily self-representations. The current study evaluated a model that hypothesized that sexual body self-representations (sexual subjectivity, self-objectification, genital self-image) explain (i.e., mediate) the relation between internalized working models of parent-child relationships (attachment, separation-individuation, parental identification) and sexual desire in heterosexual women. We recruited 614 young, heterosexual women (M = 25.5 years, SD = 4.63) through social media. The women completed an online survey. Structural equation modeling was used. The hypotheses were supported in that the relation between internalized working models of parent-child relationships (attachment and separation-individuation) and sexual desire was mediated by sexual body self-representations (sexual body esteem, self-objectification, genital self-image). However, parental identification was not related significantly to sexual body self-representations or sexual desire in the model. Current findings demonstrated that understanding female sexual desire necessitates considering women's internalized working models of early parent-child relationships and their experiences of their bodies in a sexual context. Treatment of low or absent desire in women would benefit from modalities that emphasize early parent-child relationships as well as interventions that foster mind-body integration.

[Correlation between parameters on the shape of body and dissatisfaction against it from parents among children and adolescents].

PubMed

Fu, Lianguo; Wang, Haijun; Sun, Lili; Yang, Yide; Li, Xiaohui; Wang, Shuo; Meng, Xiangkun; Wang, Zhenghe; Ma, Jun

2015-04-01

To analyze the correlation between children and adolescents' body shape parameters and parent's dissatisfaction on it. Stratified cluster sampling method was used to select students and their parents, and height, weight, waist circumference (WC), hip circumference (HC), skinfold thichness of the students were measured. Body image from parents was studied through the 'Ma body figural shape'. Correlation between body shape parameters and dissatisfaction towards them from the parents was analyzed under both simple- and multiple-level methods. The overall prevalence of dissatisfaction on body-shapes from parents was 69.0%, including 28.6% of the parents expecting children to be fat (PEBF) while, 40.4% of the parents expecting their children to be thin (PEBT). In males, parameters as height, weight, WC, HC, skin fold thickness, BMI in PEBT were 1.9 cm, 11.9 kg, 13.2 cm, 8.8 cm, 32.3 mm, 4.7 kg/m² respectively, all higher than the satisfaction from the parents (PBIS) (all P < 0.05), and these parameters were 2.3 cm, 7.1 kg, 7.2 cm, 5.8 cm, 14.1 mm, 2.3 kg/m² higher in PBIS than that of PEBF, respectively (all P < 0.05). In females, parameters as weight, WC, HC, skinfold thickness, BMI in PEBT appeared to be 8.6 kg, 9.1 cm, 6.6 cm, 21.9 mm, 3.5 kg/m² higher than that of PBIS (all P < 0.01), and were 5.5 kg, 5.9 cm, 5.4 cm, 10.4 mm, 1.8 kg/m² higher in PBIS than that of PEBF, respectively, plus the difference of height was 3.6 cm more (P < 0.01). Differences of body shape on parameters between PEBT and PBIS were larger in primary school students than in middle school students. However, the differences of body shape parameters between PBIS and PEBF appeared higher in middle school students than in primary school male students, but were higher in female students in primary than in middle school students. The prevalence of body dissatisfaction related to children and adolscents' body shape parameters from parents was high. Parents in the PEBT group seemed to have paid more attention to children's body shape parameters at low age. However, parents in PEBF group might have paid more attention to children's body shape parameters at high age in males or at low age in females.

Distal and Proximal Parenting as Alternative Parenting Strategies during Infants' Early Months of Life: A Cross-Cultural Study

ERIC Educational Resources Information Center

Keller, Heidi; Borke, Joern; Staufenbiel, Thomas; Yovsi, Relindis D.; Abels, Monika; Papaligoura, Zaira; Jensen, Henning; Lohaus, Arnold; Chaudhary, Nandita; Lo, Wingshan; Su, Yanjie

2009-01-01

Cultures differ with respect to parenting strategies already during infancy. Distal parenting, i.e., face-to-face context and object stimulation, is prevalent in urban educated middle-class families of Western cultures; proximal parenting, i.e., body contact and body stimulation, is prevalent in rural, low-educated farmer families. Parents from…

Child's Weight Status and Parent's Response to a School-Based Body Mass Index Screening and Parent Notification Program

ERIC Educational Resources Information Center

Lee, Jiwoo; Kubik, Martha Y.

2015-01-01

This study examined the response of parents of elementary school-aged children to a school-based body mass index (BMI) screening and parent notification program conducted in one Minnesota school district in 2010-2011 and whether parent's response was moderated by child's weight status. Randomly selected parents (N = 122) of second- and…

Perceived parenting behaviours predict young adolescents' nutritional intake and body fatness.

PubMed

Kim, Mi-Jeong; McIntosh, William A; Anding, Jenna; Kubena, Karen S; Reed, Debra B; Moon, Gap-Soon

2008-10-01

This study investigated whether perceptions of parenting behaviours predict young adolescents' nutritional intake and body fatness. The randomly selected study sample consisted of 106 13-15 years olds from Houston Metropolitan Statistical Area. Parenting style variables were created by cluster analysis and factor analysis. A two-cluster solution for both maternal and paternal parenting style represented authoritative vs. non-authoritative parenting. Two parenting dimension factors derived were maternal/paternal nurturing and control. For adolescents' energy and nutrient intake, greater maternal nurturing appeared to be most beneficial given its association with lower consumption of total kilocalorie and lower saturated fat intake. Paternal nurturing was associated with lower sodium intake, whereas paternal control predicted lower percentage of kilocalories from carbohydrate and percentage Dietary Reference Intake for dietary fibre, and greater percentage of kilocalories from total fat. Maternal authoritative parenting and lower maternal control over their adolescents may have protective effects against having heavier and fatter adolescents given their associations with adolescents' body weight, sub-scapular skinfold, waist circumference, body mass index, and the tendencies of being at risk of overweight and being overweight. None of paternal parenting styles or dimensions appeared to be significantly related to adolescents' body fatness.

Vesta Thermal Models

NASA Astrophysics Data System (ADS)

Formisano, M.; Federico, C.; Coradini, A.; Carli, C.; Turrini, D.

2011-12-01

Vesta is one of the largest Main Belt asteroid, considered the parent of the HED (Howardite - Eucrite - Diogenite) meteorites. Spectroscopic studies in fact show the presence of the 0.9 and 1.9 μm absorption bands for pyroxene in the spectra of Vesta that match those observed in the spectra of HED meteorites (see Gaffey, 1997, Surface Lihologic Heterogeneity of Asteroid 4 Vesta, Icarus, 127). The spectral connection between Vesta and the Howardite-Eurcrite-Diogenite (HED) suite of meteorites suggests that Vesta formed very early in the history of the Solar System and differentiated on a Ma-long timescale due to the decay of short-lived radioactive nuclides (see Keil K., 2002, Geological History of Asteroid 4 Vesta: The Smallest Terrestrial Planet. Asteroids III, and references therein). The importance of studying the thermal evolution of Vesta is therefore linked to the understanding of the processes of core and crust formation in planetary bodies so Vesta can be considered a good model for the primordial stages of the terrestrial planets. Our interest is mainly focused on the study of different energy sources, and how they contribute to differentiation and, more generally, to the thermal history of the body. We analyze not only the contribution of short-lived radionuclides, i.e. 26Al and 60Fe, but also the contribution of long-lived radionuclides, in particular 40K, 232Th, 235U and 238U, and that of accretional heating. The contribution of the long-lived radionuclides does not change the overall thermal history but it only slows down the cooling of the body. We have also observed that the effect of the accretional heating is limited if not negligible: in the most favourable scenarios its contribution only raise the starting temperature of the body but it is not sufficient to start the differentiation process. Vesta thermal and structural evolution is therefore characterized by the contribution of the short-lived radionuclides. The scenarios we considered differ in the time delay Δt. The time delay Δt is a parameter that takes into account not only the uncertainties due to the injection of 26Al in the Solar Nebula, but also the uncertainties linked to the time of the accretional process of Vesta. In all the scenarios we observe the differentiation of the body, i.e. the formation of a metallic core (mainly iron) and a silicatic crust of which we discuss the chemical and physical evolution, in particular by analyzing the link with the Jovian Early Bombardment phase ( D.Turrini, G.Magni, A.Coradini, 2011, Probing the history of Solar System through the cratering records on Vesta and Ceres, MNRAS, DOI: 10.1111/j.1365-2966.2011.18316.x). We also preliminarly discuss the heat released by the impacts during the Jovian Early Bombardment phase and their possible contribution to the thermal history of Vesta.

Parental Characteristics Have a Larger Effect on Children's Health Behaviour than Their Body Weight

PubMed Central

Drenowatz, Clemens; Erkelenz, Nanette; Wartha, Olivia; Brandstetter, Susanne; Steinacker, Jürgen M.

2014-01-01

Objective Parents take an important role in a child's development, but there is currently limited information on parental correlates with children's health behaviour. The purpose of this study, therefore, was to examine whether parental characteristics, such as body weight, TV consumption and sport participation, affect children's body weight and health behaviour. Methods To examine the effects of parental characteristics on children's body weight and health behaviour, baseline data of 1,118 elementary school children (7.6 ± 0.4 years) participating in a school-based intervention in southwest Germany was used. Children's height and weight were measured and parent as well as child behaviour was assessed via questionnaire. Results BMI percentiles of children were positively associated with parental BMI (r = 0.2, p < 0.01). Further, high parental TV time increased the odds for high TV time in children (ORmother = 2.2, ORfather = 2.3) and parental club sport participation increased the odds for club sport participation in children (ORmother = 1.9, ORfather = 1.7). The relationship between parental and child behaviour was stronger than the relationship between parental BMI and BMI percentiles of the child. Conclusion These results suggest that parental behaviour and role modelling provide an important contribution to childrens’ health behaviour, especially at younger ages. PMID:25434370

Parental characteristics have a larger effect on children's health behaviour than their body weight.

PubMed

Drenowatz, Clemens; Erkelenz, Nanette; Wartha, Olivia; Brandstetter, Susanne; Steinacker, Jürgen M

2014-01-01

Parents take an important role in a child's development, but there is currently limited information on parental correlates with children's health behaviour. The purpose of this study, therefore, was to examine whether parental characteristics, such as body weight, TV consumption and sport participation, affect children's body weight and health behaviour. To examine the effects of parental characteristics on children's body weight and health behaviour, baseline data of 1,118 elementary school children (7.6 ± 0.4 years) participating in a school-based intervention in southwest Germany was used. Children's height and weight were measured and parent as well as child behaviour was assessed via questionnaire. BMI percentiles of children were positively associated with parental BMI (r = 0.2, p <0.01). Further, high parental TV time increased the odds for high TV time in children (OR mother= 2.2, OR father = 2.3) and parental club sport participation increased the odds for club sport participation in children (OR mother = 1.9, OR father = 1.7). The relationship between parental and child behaviour was stronger than the relationship between parental BMI and BMI percentiles of the child. These results suggest that parental behaviour and role modeling provide an important contribution to childrens' health behaviour, especially at younger ages.

Simulations of Collisional Disruption at the Catastrophic Impact Energy Threshold: Effect of the Target's Internal Structure and Diameter

NASA Astrophysics Data System (ADS)

Michel, P.; Benz, W.; Richardson, D. C.

2005-08-01

Recent simulations of asteroid break-ups, including both the fragmentation of the parent body and the gravitational interactions of the fragments, have allowed to reproduced successfully the main properties of asteroid families formed in different regimes of impact energy. Here, using the same kind of simulations, we concentrate on a single regime of impact energy, the so-called catastrophic threshold usually designated by Qcrit, which results in the escape of half of the target's mass. Considering a wide range of diameter values and two kinds of internal structures of the parent body, monolithic and pre-shattered, we analyse their potential influences on the value of Qcrit and on the collisional outcome limited here to the fragment size and ejection speed distributions, which are the main outcome properties used by collisional models to study the evolutions of the different populations of small bodies. For all the considered diameters and the two internal structures of the parent body, we confirm that the process of gravitational reaccumulation is at the origin of the largest remnant's mass. We then find that, for a given diameter of the parent body, the impact energy corresponding to the catastrophic disruption threshold is highly dependent on the internal structure of the parent body. In particular, a pre-shattered parent body containing only damaged zones but no macroscopic voids is easier to disrupt than a monolithic parent body. Other kinds of internal properties that can also characterize small bodies in real populations will be investigated in a future work.

Selection on parental performance opposes selection for larger body mass in a wild population of blue tits.

PubMed

Thomson, Caroline E; Bayer, Florian; Crouch, Nicholas; Farrell, Samantha; Heap, Elizabeth; Mittell, Elizabeth; Zurita-Cassinello, Mar; Hadfield, Jarrod D

2017-03-01

There is abundant evidence in many taxa for positive directional selection on body size, and yet little evidence for microevolutionary change. In many species, variation in body size is partly determined by the actions of parents, so a proposed explanation for stasis is the presence of a negative genetic correlation between direct and parental effects. Consequently, selecting genes for increased body size would result in a correlated decline in parental effects, reducing body size in the following generation. We show that these arguments implicitly assume that parental care is cost free, and that including a cost alters the predicted genetic architectures needed to explain stasis. Using a large cross-fostered population of blue tits, we estimate direct selection on parental effects for body mass, and show it is negative. Negative selection is consistent with a cost to parental care, mainly acting through a reduction in current fecundity rather than survival. Under these conditions, evolutionary stasis is possible for moderately negative genetic correlations between direct and parental effects. This is in contrast to the implausibly extreme correlations needed when care is assumed to be cost-free. Thus, we highlight the importance of accounting correctly for complete selection acting on traits across generations. © 2017 The Author(s). Evolution © 2017 The Society for the Study of Evolution.

"BodyWorks": A Parent-Focused Program to Promote Healthful Eating and Physical Activity for Children and Adolescents

ERIC Educational Resources Information Center

Borden, Valerie Melino; Labiner-Wolfe, Judith; Blake, Susan M.; Marr, Amanda; Rowe, Jonelle; Wasserman, Jill

2012-01-01

The "BodyWorks" program was designed to help parents improve family eating and activity behaviors. "BodyWorks" was associated with significant gains in parents' knowledge about nutrition and activity, and greater self-efficacy to set family nutrition goals, plan physical activities, and change eating habits. (Contains 1 table.)

Towards Calibrating the Vestan Regolith: Correlating the Petrology, Chemistry and Spectroscopy of Howardites

NASA Technical Reports Server (NTRS)

Mittlefehldt, D. W.; Ammannito, E.; Hiroi, T.; De Angelis, S.; Di Iorio, T.; Pieters, C. M.; De Sanctis, C.

2013-01-01

The Dawn spacecraft carries a visible and infrared mapping spectrometer (VIR) [1] that has acquired spectra for the wavelength range 0.25-5.0 µm at various spatial resolutions covering much of the vestan surface [2]. Through comparison of VIR spectra with laboratory spectra of howardite, eucrite and diogenite meteorites, the distribution of more diogenite-rich and more eucrite-rich terranes on Vesta have been mapped [3], but these maps are qualitative in nature. The available laboratory spectra are not well-integrated with detailed sample petrology or composition limiting their utility for lithologic mapping. Importantly, howardites are now recognized to come in two subtypes, regolithic and fragmental [4]. The former are breccias assembled in part from true regolith, while the latter have had much less exposure to the space environment. We are attempting to develop a more quantitative basis for mapping the distribution of lithologic types on Vesta through acquiring laboratory spectra on splits of howardites that have been petrologically and chemically characterized [5]. Noble gas analyses have been done on some allowing identification of those howardites that have been exposed in the true regolith of Vesta [6].

Beneficiation of lunar ilmenite

NASA Technical Reports Server (NTRS)

Ruiz, Joaquin

1991-01-01

One of the most important commodities lacking in the moon is free oxygen which is required for life and used extensively for propellent. Free oxygen, however, can be obtained by liberating it from the oxides and silicates that form the lunar rocks and regolith. Ilmenite (FeTiO3) is considered one of the leading candidates for production of oxygen because it can be reduced with a reasonable amount of energy and it is an abundant mineral in the lunar regolith and many mare basalts. In order to obtain oxygen from ilmenite, a method must be developed to beneficiate ilmenite from lunar material. Two possible techniques are electrostatic or magnetic methods. Both methods have complications because lunar ilmenite completely lacks Fe(3+). Magnetic methods were tested on eucrite meteorites, which are a good chemical simulant for low Ti mare basalts. The ilmenite yields in the experiments were always very low and the eucrite had to be crushed to xxxx. These data suggest that magnetic separation of ilmenite from fine grain lunar basalts would not be cost effective. Presently, experiments are being performed with electrostatic separators, and lunar regolith is being waited for so that simulants do not have to be employed.

Parent Reactions to a School-Based Body Mass Index Screening Program

ERIC Educational Resources Information Center

Johnson, Suzanne Bennett; Pilkington, Lorri L.; Lamp, Camilla; He, Jianghua; Deeb, Larry C.

2009-01-01

Background: This study assessed parent reactions to school-based body mass index (BMI) screening. Methods: After a K-8 BMI screening program, parents were sent a letter detailing their child's BMI results. Approximately 50 parents were randomly selected for interview from each of 4 child weight-classification groups (overweight, at risk of…

Preferred child body size and parental underestimation of child weight in Mexican American families

PubMed Central

Pasch, Lauri A.; Penilla, Carlos; Tschann, Jeanne M.; Martinez, Suzanna M.; Deardorff, Julianna; de Groat, Cynthia L.; Gregorich, Steven E.; Flores, Elena; Butte, Nancy F.; Greenspan, Louise C.

2016-01-01

Objective To determine whether parents who prefer a heavier child would underestimate their child's weight more than those who prefer a leaner child. Methods Participants were Mexican American families (312 mothers, 173 fathers, and 312 children ages 8-10) who were interviewed and had height and weight measurements. Parents reported their preferred child body size and their perceptions of their child's weight. Parents’ underestimation of their child's weight was calculated as the standardized difference between parent's perception of their child's weight and the child's body mass index (BMI) z-score. Demographic factors and parental BMI were also assessed. Results Although 50% of children were overweight or obese, only 11% of mothers and 10% of fathers perceived their children as being somewhat or very overweight. Multiple regressions controlling for covariates (parental BMI and child age) showed that parents who preferred a heavier child body size underestimated their children's weight more, compared to those who preferred a leaner child (β for mothers = .13, p < .03; (β for fathers = .17, p < .03). Conclusions for Practice Parents who preferred a heavier child body size underestimated their child's weight to a greater degree than parents who preferred a leaner child. Attempts by pediatricians to correct parents’ misperceptions about child weight may damage rapport and ultimately fail if the misperception is actually a reflection of parents’ preferences, which may not be readily amenable to change. Future research should address optimal methods of communication about child overweight which take into account parent preferences. PMID:27016351

Body-size perception, body-esteem, and parenting history in college women reporting a history of child abuse.

PubMed

Eubanks, Jessica R; Kenkel, Michaela Y; Gardner, Rick M

2006-04-01

This study investigated the relations among physical, emotional, and sexual abuse up to adolescence and subsequent perception of body size, detection of changes in body size, and body-esteem. The role of parenting history in abused participants was also examined. 38 college undergraduate women, half of whom had been abused, reported instances of abuse, childhood parenting history, and current body-esteem. A recently developed software program of Gardner and Boice was used to present a series of distorted frontal profiles of each participant's own body for the women to rate as being too wide or too thin. A psychophysical procedure called adaptive probit estimation was used to measure the amount of over- and underestimation of these ratings and whether these changes were statistically significant. Analysis showed abused participants had distorted perceptions of body size, although the direction of the distortion was not consistent. There was no difference in detection of changes in body size. Abused and nonabused participants differed on measures of body-esteem and on ratings of most parenting experiences, including experiences with both mothers and fathers.

"Solar-Wind-Rich" Howardite: True Regolith vs. CM-Implanted Components

NASA Technical Reports Server (NTRS)

Cartwright, Julia A.; Mittlefehldt, D. W.; Herrin, J. S.; Hermann, S.; Ott, U.

2011-01-01

Howardite, eucrite and diogenite meteorites (collectively HED) likely originate from asteroid 4-Vesta [1], one of two asteroids targeted by NASA s Dawn mission. Many howardites (polymict breccias of E and D material) contain "regolithic" features, including impact-melt clasts, fragmental breccia clasts, and carbonaceous chondrite fragments. True regolithic nature can be determined through noble gas analysis, as Solar Wind (SW) is implanted into the upper-most surfaces of solar system bodies. Whilst previous work [2] suggested that high siderophile element contents (e.g. Ni of 300-1200 g/g) were regolith indicators, we found no obvious correlation between SW and these indicators in our initial howardite noble gas analyses [3]. We observed CM-like fragments in a number of our howardites, whose textures suggest late addition to the breccia assemblage [4]. As typical CMs contain mixtures of SW (in matrix) and planetary (in clasts) components [5], we investigate the dominance of such components in SW-rich howardites. This will help deter-mine the extent of implanted SW in HED grains vs. SW and planetary gases from CM fragments, and allow better understanding of regolith processes

Secondary-volatiles linked metallic iron in eucrites: The dual-origin metals of Camel Donga

NASA Astrophysics Data System (ADS)

Warren, Paul H.; Isa, Junko; Ebihara, Mitsuru; Yamaguchi, Akira; Baecker, Bastian

2017-04-01

The unique occurrence of abundant ( 1 vol%) near-pure-Fe metal in the Camel Donga eucrite is more complicated than previously believed. In addition to that component of groundmass metal, scattered within the meteorite are discrete nodules of much higher kamacite abundance. We have studied the petrology and composition of two of these nodules in the form of samples we call CD2 and CD3. The nodules are ovoids 11 (CD2) to 15 (CD3) mm across, with metal, or inferred preweathering metal, abundances of 12-17 vol% (CD2 is unfortunately quite weathered). The CD3 nodule also includes at its center a 5 mm ovoid clumping (6 vol%) of F-apatite. Both nodules are fine-grained, so the high Fe metal and apatite contents are clearly not flukes of inadequate sampling. The metals within the nodules are distinctly Ni-rich (0.3-0.6 wt%) compared to the pure-Fe (Ni generally 0.01 wt%) groundmass metals. Bulk analyses of three pieces of the CD2 nodule show that trace siderophile elements Ir, Os, and Co are commensurately enriched; Au is enriched to a lesser degree. The siderophile evidence shows the nodules did not form by in situ reduction of pyroxene FeO. Moreover, the nodules do not show features such as silica-phase enrichment or pyroxene with reduced FeO (as constrained by FeO/MgO and especially FeO/MnO) predicted by the in situ reduction model. The oxide minerals, even in groundmass samples well away from the nodules, also show little evidence of reduction. Although the nodule boundaries are generally sharp, groundmass-metal Ni content is anti-correlated with distance from the CD3 nodule. We infer that the nodules represent materials that originated within impactors into the Camel Donga portion of the eucrite crust, but probably were profoundly altered during later metamorphism/metasomatism. Origin of the pure-Fe groundmass metal remains enigmatic. In situ reduction probably played an important role, and association in the same meteorite of the Fe-nodules is probably significant. But the fluid during alteration was probably not (as previously modeled) purely S and O, of simple heat-driven internal derivation. We conjecture a two-stage metasomatism, as fluids passed through Camel Donga after impact heating of volatile-rich chondritic masses (survivors of gentle accretionary impacts) within the nearby crust. First, reduction to form troilite may have been triggered by fluids rich in S2 and CO (derived from the protonodules?), and then in a distinct later stage, fluids were (comparatively) H2O-rich, and thus reacted with troilite to form pure-Fe metal along with H2S and SO2. The early eucrite crust was in places a dynamic fluid-bearing environment that hosted complex chemical processes, including some that engendered significant diversity among metal+sulfide alterations.

Familial resemblance of body composition, physical activity, and resting metabolic rate in pre-school children

PubMed Central

Djafarian, Kurosh; Speakman, John R; Stewart, Joanne; M Jackson, Diane

2013-01-01

Background: Although parental obesity is a well-established predisposing factor for the development of obesity, associations between regional body compositions, resting metabolic rates (RMR), and physical activity (PA) of parents and their pre-school children remain unknown. The objective of this study was to investigate parent-child correlations for total and regional body compositions, resting energy expenditures, and physical activity. Methods: Participants were 89 children aged 2-6 years and their parents, consisting of 61 families. Resting metabolic rate was assessed using indirect calorimetry. Total and regional body compositions were measured by both dual energy X-ray absorptiometry (DXA) and deuterium dilution. Physical activity was assessed by an accelerometer. Results: There was a significant parent-offspring regression for total fat free mass (FFM) between children and their mothers (P=0.02), fathers (P=0.02), and mid-parent (average of father and mother value) (P=0.002) when measured by DXA. The same was true for fat mass (FM) between children and mothers (P<0.01), fathers (P=0.02), and mid-parent (P=0.001). There was no significant association between children and parents for physical activity during the entire week, weekend, weekdays, and different parts of days, except for morning activity, which was positively related to the mothers’ morning activities (P<0.01) and mid-parent (P=0.009). No association was found between RMR of children and parents before and after correction for FFM and FM. Conclusion: These data suggest a familial resemblance for total body composition between children and their parents. Our data showed no familial resemblance for PA and RMR between children and their parents. PMID:26989715

Relation of attitude toward body elimination to parenting style and attitude toward the body.

PubMed

Corgiat, Claudia A; Templer, Donald I

2003-04-01

The purpose was to estimate the relation of attitude toward body elimination in 93 college students (27 men and 66 women), to authoritarian personality features, participants' perception of their mothers' parenting style, and attitudes toward cleanliness, sex, and family nudity. Subjects were administered the Body Elimination Attitude Scale, the Four-item F Scale, the Parental Authority Questionnaire Pertaining to Mothers, and the items "Sex is dirty," "Cleanliness is next to godliness," and "Children should never see other family members nude." Larger scores for disgust toward body elimination were associated with authoritarian personality characteristics, being less likely to describe mother's parenting style as authoritative (open communication) and more likely to describe it as authoritarian and lower scores for tolerance for family nudity. Implications for further research were suggested.

Factors associated with parental use of restrictive feeding practices to control their children's food intake.

PubMed

Gray, Wendy N; Janicke, David M; Wistedt, Kristin M; Dumont-Driscoll, Marilyn C

2010-10-01

There is a critical need to identify risk factors that make parents more likely to restrict their child's food intake. Child weight and ethnicity, parent weight, parent body dissatisfaction, and parent concern of child weight were examined as correlates of parent use of restrictive feeding practices in a diverse sample of 191 youth (ages 7-17). Participants attending a pediatric outpatient visit completed the Child Feeding Questionnaire (parent feeding practices and beliefs), the Figure Rating Scale (body dissatisfaction) and a demographic form. Parent BMI and child degree of overweight were calculated. Parent use of restrictive feeding practices was positively associated with parent BMI and was moderated by parent body dissatisfaction. Parent concern of child weight mediated the relationship between increasing child degree of overweight and parent use of restrictive feeding practices. There were no differences by child gender or ethnicity in parent use of restrictive feeding practices. These preliminary findings highlight the importance of assessing for underlying parent motivations for utilizing restrictive feeding practices and may help to identify and intervene with families at-risk for engaging in counterproductive weight control strategies. Continued identification of correlates of parent use of restrictive feeding practices is needed across child development and among individuals from diverse backgrounds.

Controlling parental feeding practices and child body composition in ethnically and economically diverse preschool children.

PubMed

Wehrly, Sarah E; Bonilla, Chantal; Perez, Marisol; Liew, Jeffrey

2014-02-01

Controlling parental feeding practices may be associated with childhood overweight, because coercive or intrusive feeding practices may negatively impact children's development of self-regulation of eating. This study examined pressuring or forcing a child (healthy or unhealthy foods) and restricting child from unhealthy or snack foods as two types of controlling feeding practices that explain unique variances in measures of child body composition (BMI, percent body fat, and parental perception of child weight). In an ethnically and economically diverse sample of 243 children aged 4-6years old and their biological parents (89% biological mothers, 8% biological fathers, and 3% step or grand-parent), descriptive statistics indicate ethnic and family income differences in measures of feeding practices and child body composition. Additionally, the two "objective" indices of body composition (BMI and percent body fat) were related to low pressure to eat, whereas the "subjective" index (perceived child weight) was related to restriction. Regression analyses accounting for ethnic and family income influences indicate that pressure to eat and restriction both explained unique variances in the two "objective" indices of body composition, whereas only restriction explained variance in perceived child weight. Findings have implications for helping parents learn about feeding practices that promote children's self-regulation of eating that simultaneously serves as an obesity prevention strategy. Copyright © 2013 Elsevier Ltd. All rights reserved.

The Grand Geochemistry of 4 Vesta: First Results

NASA Technical Reports Server (NTRS)

Prettyman, T. H.; Beck, A.; Feldman, W. C.; Forni, O.; Joy, S. P.; Lawrence, D. J.; McCoy T. J.; McFadden, L. A.; McSween, H. Y.; Mittlefehldt, D. W.;

Perception of body image of adolescents and of their parents in relation to the nutritional status and blood pressure.

PubMed

Silveira Vieira, Raquel; Dal Bosco, Simone Morelo; Grave, Magali Trezinha Quevedo; Adami, Fernanda Scherer

2015-04-01

The perception of body image of adolescents is an instrument for nutritional assessment to health conditions. To verify the body image perception of adolescents and their parents in relation to nutritional status and blood pressure levels. Population-based study, and cross-sectional model, conducted with parents and adolescents aged 10-19 years old, in rural and urban zones in public schools. There was applied the Scale silhouettes for parents about the perception of the described body image and a question about the concern of the nutritional status of their children. There were verified the blood pressure, weight, height and waist circumference, the BMI (kg/m²) calculation of the adolescents, and the self-perceived body image. The data was expressed as average ± standard deviation and percentages. The sample consisted of 914 adolescents with a mean age of 13.12 ± 2.17 years, 56.8% female and 68.9% were eutrophic. As for blood pressure levels, 17.6% were classified in pre-hypertensive, 18.8% in stage 1 hypertension and 6% in stage 2. About the self-perception, 68% considered themselves being eutrophic and 64.75% of the parents classified their children as eutrophic. There was observed a direct and significant correlation among the body mass index, waist circumference, weight, systemic and diastolic blood pressure with the self-perception of the adolescents and the body image perceptions of the parents (p<0.001). The nutritional status was significantly correlated with blood pressure, waist circumference and body image perceptions of the adolescents and their respective parents. Copyright AULA MEDICA EDICIONES 2014. Published by AULA MEDICA. All rights reserved.

Bodies as evidence: Mapping new terrain for teen pregnancy and parenting.

PubMed

Gubrium, Aline C; Fiddian-Green, Alice; Jernigan, Kasey; Krause, Elizabeth L

2016-01-01

Predominant approaches to teen pregnancy focus on decreasing numbers of teen mothers, babies born to them, and state dollars spent to support their families. This overshadows the structural violence interwoven into daily existence for these young parents. This paper argues for the increased use of participatory visual methods to compliment traditional research methods in shifting notions of what counts as evidence in response to teen pregnancy and parenting. We present the methods and results from a body mapping workshop as part of 'Hear Our Stories: Diasporic Youth for Sexual Rights and Justice', a project that examines structural barriers faced by young parenting Latinas and seeks to develop relevant messaging and programming to support and engage youth. Body mapping, as an engaging, innovative participatory visual methodology, involves young parenting women and other marginalised populations in drawing out a deeper understanding of sexual health inequities. Our findings highlight the ways body mapping elicits bodies as evidence to understand young motherhood and wellbeing.

Small-scale dust structures in Halley's coma. II. Disintegration of large dust bodies

NASA Astrophysics Data System (ADS)

Oberc, P.

2004-10-01

Small-scale dust structures, SDSs, altogether ˜35 events with extent ˜30-220 km, have been recognized owing to electric field records, mostly near the closest approach of Vega-2 to Halley's nucleus. Several (8-9) morphological forms of SDS have been identified, and all they make one family. Among the family members, the key form (with respect to which, all other forms can be regarded as degenerate) is a sequence of 3-5 dust clouds. The morphological forms represent various Vega-2 passes through SDSs at different stages of development. SDSs observable as the key form consisted of several fairly regularly spaced dust subpopulations, whose plane of symmetry was parallel to the comet orbit plane. That regularity together with specific features of morphological forms strongly constrain disintegration scenarios and dynamics of fragments, and allow to draw a number of conclusions, the main of which are: SDS parent bodies were ice-free dust aggregates lifted from the nucleus near the comet perihelion, whose masses were in the range ˜0.1-1 of the biggest emitted mass (mass of a body accelerated to the escape velocity, i.e., ˜300-1500 kg); the disintegration scenario comprised a few steps, and the first-step disintegration consisted mainly in consecutive detachments of biggest first-step fragments (BF-SFs) from the parent body; a SDS observable as the key form included the dust minitail of parent body and a few BF-SF minitails, the former one being longer than the latter ones; SDS parent bodies had a fractal-like internal structure, and the BF-SF mass was a few percent of the parent body mass; the thermal conductivity of SDS parent body was less than ˜0.4 W m -1 K -1 or so, while the latent heat of gluing organics was roughly 80 kJ mol -1; the disintegration mechanism was a combination of sintering and sublimation of organics. The multistep disintegration of SDS parent bodies can be reconciled with the basically one-step disintegration of aggregates responsible for the dust boundary (Oberc, P., Icarus 1996, 124, 195-208). The fractal-like structure and the relation between BF-SF mass and parent body mass are in agreement with predictions from the Weidenschilling model of comet formation. Large ice-free dust bodies, in particular SDS parent bodies, can be identified with refractory boulders postulated by some comet nucleus models.

Modes of planetary-scale Fe isotope fractionation

NASA Astrophysics Data System (ADS)

Schoenberg, Ronny; von Blanckenburg, Friedhelm

2006-12-01

A comprehensive set of high-precision Fe isotope data for the principle meteorite types and silicate reservoirs of the Earth is used to investigate iron isotope fractionation at inter- and intra-planetary scales. 14 chondrite analyses yield a homogeneous Fe isotope composition with an average δ56Fe/ 54Fe value of - 0.015 ± 0.020‰ (2 SE) relative to the international iron standard IRMM-014. Eight non-cumulate and polymict eucrite meteorites that sample the silicate portion of the HED (howardite-eucrite-diogenite) parent body yield an average δ56Fe/ 54Fe value of - 0.001 ± 0.017‰, indistinguishable to the chondritic Fe isotope composition. Fe isotope ratios that are indistinguishable to the chondritic value have also been published for SNC meteorites. This inner-solar system homogeneity in Fe isotopes suggests that planetary accretion itself did not significantly fractionate iron. Nine mantle xenoliths yield a 2 σ envelope of - 0.13‰ to + 0.09‰ in δ56Fe/ 54Fe. Using this range as proxy for the bulk silicate Earth in a mass balance model places the Fe isotope composition of the outer liquid core that contains ca. 83% of Earth's total iron to within ± 0.020‰ of the chondritic δ56Fe/ 54Fe value. These calculations allow to interprete magmatic iron meteorites ( δ56Fe/ 54Fe = + 0.047 ± 0.016‰; N = 8) to be representative for the Earth's inner metallic core. Eight terrestrial basalt samples yield a homogeneous Fe isotope composition with an average δ56Fe/ 54Fe value of + 0.072 ± 0.016‰. The observation that terrestrial basalts appear to be slightly heavier than mantle xenoliths and that thus partial mantle melting preferentially transfers heavy iron into the melt [S. Weyer, A.D. Anbar, G.P. Brey, C. Munker, K. Mezger and A.B. Woodland, Iron isotope fractionation during planetary differentiation, Earth and Planetary Science Letters 240(2), 251-264, 2005.] is intriguing, but also raises some important questions: first it is questionable whether the Fe isotope composition of lithospheric mantle xenoliths are representative for an undisturbed melt source, and second, HED and SNC meteorites, representing melting products of 4Vesta and Mars silicate mantles would be expected to show a similar fractionation towards heavy isotope compositions. This is not observed. Four international granitoid standards with SiO 2 contents between 60 and 70 wt.% yield δ56Fe/ 54Fe values between 0.118‰ and 0.132‰. An investigation of the alpine Bergell igneous rock suite revealed a positive correlation between Fe isotope compositions and SiO 2 contents — from gabbros and tonalites ( δ56Fe/ 54Fe ≈ 0.03 to 0.09‰) to granodiorites and silicic dykes ( δ56Fe/ 54Fe ≈ 0.14 to 0.23‰). Although in this suite δ56Fe/ 54Fe correlates with δ18O values and radiogenic isotopes, open-system behavior to explain the heavy iron is not undisputed. This is because an obvious assimilant with the required heavy Fe isotope composition has so far not been identified. Alternatively, the relatively heavy granite compositions might be obtained by fractional crystallisation of the melt. Ultimately, further detailed studies on natural rocks and the experimental determination of mineral/melt fractionation factors at magmatic conditions are required to unravel whether or not iron isotope fractionation takes place during partial mantle melting and crystal fractionation.

My Body, My Weight: Body Perception Among African American and Caucasian First-Graders and Their Parents

DTIC Science & Technology

2003-10-02

Self by BMI Table 14a. African American Mothers’ Body Satisfaction for Self by BMI Table 15. Mothers’ Body Satisfaction for Their Children by Race...Table 16. Caucasian Mothers’ Body Satisfaction for Their Children by Child BMI ix Table 17. Mothers’ Body Satisfaction for Self and Child by Parent...controlling for mother BMI . Because the present data suggested that mothers’ perceived current body size, ideal

The role of S in the evolution of the parental cores of the iron meteorites

NASA Technical Reports Server (NTRS)

Kracher, A.; Wasson, J. T.

1982-01-01

The S contents of iron meteorite parent bodies are estimated on the basis of cosmochemical relationships to undifferentiated meteorites, the results are compared to observations on the major magmatic iron meteorite groups, and evidence is presented that S/Ni ratios in their parent melts were much lower than those inferred for the parent body. Several alternative models to account for the discrepancy are offered, including volatilization of S from the IIAB parent body, liquid immiscibility, and metastable liquid layers produced by episodic melting. Finally, the fate of the S-rich meteoroidal material is discussed, as well as the question of why it seems to be missing from meteorite collections.

Indulgent feeding style and children's weight status in preschool.

PubMed

Hughes, Sheryl O; Shewchuk, Richard M; Baskin, Monica L; Nicklas, Theresa A; Qu, Haiyan

2008-10-01

The primary aim of this study was to examine whether parent affect and child temperament characteristics differ across feeding styles in low-income families, given suggestive evidence. The secondary aim was to examine whether feeding styles were still related to children's body mass index independent of parent affect, child temperament, and known correlates. Participants in this study were 718 parents of children attending Head Start programs across two sites (Texas and Alabama). Parents were categorized into feeding styles of authoritative (n = 118), authoritarian (n = 219), indulgent (n = 240) and uninvolved (n = 141) using a parent-report questionnaire characterizing feeding in a general parenting paradigm. Parents completed questionnaires and measured height and weight was obtained from parents and children. Differences were found across feeding styles on parent affect and child temperament characteristics. Indulgent parents reported lower Negative Affect for themselves and lower Negative Affectivity for their children. The indulgent feeding style was significantly associated with higher child body mass index after controlling for parent affect, child temperament, and correlates (ethnicity, child age, parent body mass index). The results of this study not only show a robust association between the indulgent feeding style and weight status of low-income preschool children, but also suggest how congruence between parent emotional affect and child temperament characteristics may contribute to excess consumption among children of indulgent parents.

Aerodynamic Analysis of Tektites and Their Parent Bodies

NASA Technical Reports Server (NTRS)

Adams, E. W.; Huffaker, R. M.

1962-01-01

Experiment and analysis indicate that the button-type australites were derived from glassy spheres which entered or re-entered the atmosphere as cold solid bodies; in case of average-size specimens, the entry direction was nearly horizontal and the entry speed between 6.5 and 11.2 km/sec. Terrestrial origin of such spheres is impossible because of extremely high deceleration rates at low altitudes. The limited extension of the strewn fields rules out extraterrestrial origin of clusters of such spheres because of stability considerations for clusters in space. However, tektites may have been released as liquid droplets from glassy parent bodies ablating in the atmosphere of the earth. The australites then have skipped together with the parent body in order to re-enter as cold spheres. Terrestrial origin of a parent body would require an extremely violent natural event. Ablation analysis shows that fusion of opaque siliceous stone into glass by aerodynamic heating is impossible.

FT-IR and µ-IR characterization of HED meteorites in relation to infrared spectra of Vesta-like asteroids

NASA Astrophysics Data System (ADS)

Ferrari, M.; Dirri, F.; Palomba, E.; Stefani, S.; Longobardo, A.; Rotundi, A.

2017-09-01

We present the results of the FT-IR and µ-IR study of three Howardite-Eucrite-Diogenite meteorites (HEDs) compared to the spectroscopic data collected by VIR onboard Dawn spacecraft. The origin of this group of achondrites is thought to be linked to the asteroid 4 Vesta, hypothesis lately reinforced by the data provided by the Dawn mission.

Vesta Mineralogy: VIR maps Vesta's surface

NASA Technical Reports Server (NTRS)

Coradina, A.; DeSanctis, M.; Ammannito, E.; Capaccioni, F.; Capria, T.; Carraro, F.; Cartacci, M.; Filacchione, G.; Fonte, S.; Magni, G.;

The structure of the asteroid 4 Vesta as revealed by models of planet-scale collisions.

PubMed

Jutzi, M; Asphaug, E; Gillet, P; Barrat, J-A; Benz, W

2013-02-14

Asteroid 4 Vesta seems to be a major intact protoplanet, with a surface composition similar to that of the HED (howardite-eucrite-diogenite) meteorites. The southern hemisphere is dominated by a giant impact scar, but previous impact models have failed to reproduce the observed topography. The recent discovery that Vesta's southern hemisphere is dominated by two overlapping basins provides an opportunity to model Vesta's topography more accurately. Here we report three-dimensional simulations of Vesta's global evolution under two overlapping planet-scale collisions. We closely reproduce its observed shape, and provide maps of impact excavation and ejecta deposition. Spiral patterns observed in the younger basin Rheasilvia, about one billion years old, are attributed to Coriolis forces during crater collapse. Surface materials exposed in the north come from a depth of about 20 kilometres, according to our models, whereas materials exposed inside the southern double-excavation come from depths of about 60-100 kilometres. If Vesta began as a layered, completely differentiated protoplanet, then our model predicts large areas of pure diogenites and olivine-rich rocks. These are not seen, possibly implying that the outer 100 kilometres or so of Vesta is composed mainly of a basaltic crust (eucrites) with ultramafic intrusions (diogenites).

The structure of the asteroid 4 Vesta as revealed by models of planet-scale collisions

NASA Astrophysics Data System (ADS)

Jutzi, M.; Asphaug, E.; Gillet, P.; Barrat, J.-A.; Benz, W.

2013-02-01

Asteroid 4 Vesta seems to be a major intact protoplanet, with a surface composition similar to that of the HED (howardite-eucrite-diogenite) meteorites. The southern hemisphere is dominated by a giant impact scar, but previous impact models have failed to reproduce the observed topography. The recent discovery that Vesta's southern hemisphere is dominated by two overlapping basins provides an opportunity to model Vesta's topography more accurately. Here we report three-dimensional simulations of Vesta's global evolution under two overlapping planet-scale collisions. We closely reproduce its observed shape, and provide maps of impact excavation and ejecta deposition. Spiral patterns observed in the younger basin Rheasilvia, about one billion years old, are attributed to Coriolis forces during crater collapse. Surface materials exposed in the north come from a depth of about 20 kilometres, according to our models, whereas materials exposed inside the southern double-excavation come from depths of about 60-100 kilometres. If Vesta began as a layered, completely differentiated protoplanet, then our model predicts large areas of pure diogenites and olivine-rich rocks. These are not seen, possibly implying that the outer 100 kilometres or so of Vesta is composed mainly of a basaltic crust (eucrites) with ultramafic intrusions (diogenites).

Dynamic crystallization of a eucrite basalt. [achondrite textural features produced by superheating and differing cooling rates

NASA Technical Reports Server (NTRS)

Walker, D.; Powell, M. A.; Hays, J. F.; Lofgren, G. E.

1978-01-01

The textural features produced in Stannern, a non-porpyritic representative of the eucrite basaltic achondrite class of meteorite, at differing cooling rates and various degrees of initial superheating were studied. Textures produced from mildly superheated melts were found to be fasciculate rather than porphyritic as the result of the cosaturated bulk chemistry of Stannern. The qualitative type of texture apparently depends mainly on the degree of initial superheating, whereas cooling rate exerts a strong influence on the coarseness of texture. Increasing the degree of superheating produces textures from intergranular/subophitic to fasciculate/porphyritic. With initial superheating to 1200 deg C the transition to quasi-porphyritic is controlled by cooling rate, but the development of phenocrysts is merely an overprint on the fasciculate background texture of the groundmass. The suppression of fasciculate texture is completed by a decrease of the degree of initial superheating below the plagioclast entry and suppression of quasi-porphyritic texture is completed by decrease of the degree of initial superheating below pyroxene entry; these qualitative changes do not seem to be produced by changes of cooling rate. A grain size/cooling rate dependence has been used to deduce the cooling rate of fasciculate-textured Stannern clasts (10.1 to 100 deg C/hr).

Reassessing the Formation of CK7 Northwest Africa (NWA) 8186

NASA Technical Reports Server (NTRS)

Srinivasan, P.; McCubbin, F. M.; Lapen, T. J.; Righter, M.; Agee, C. B.

2017-01-01

The classification of meteorites is commonly determined using isotopes, modal mineralogy, and bulk compositions [1]. Bulk rare earth elements (REEs) in meteorites are additionally utilized to understand parent body processes. Numerous authors have shown that chondritic groups exhibit REE patterns that may be attributable to their parent bodies [e.g. 2-4], and variations in abundances and concentrations of REEs may reflect early nebular processes, thermal metamorphism, and aqueous alteration on the parent body [5-6].

Correlates of parental feeding practices with pre-schoolers: Parental body image and eating knowledge, attitudes, and behaviours.

PubMed

Damiano, Stephanie R; Hart, Laura M; Paxton, Susan J

2016-06-01

Parental feeding practices have been linked to eating and weight status in young children; however, more research is needed to understand what influences these feeding practices. The aim of this study was to examine how parental feeding practices that are linked to unhealthy eating patterns in young children, are related to parental body image and eating knowledge, attitudes, and behaviours . Participants were 330 mothers of a 2- to 6-year-old child. Mothers completed measures of knowledge of child body image and eating patterns, overvaluation of weight and shape, internalization of general media and athletic ideals, dieting, and parental feeding practices. Higher maternal knowledge of strategies to promote positive child body image and eating patterns predicted lower weight restriction, instrumental, emotional, and pushing to eat feeding practices. Overvaluation of weight and shape predicted use of fat restriction. Maternal internalization of the athletic ideal predicted instrumental and pushing to eat feeding practices. As these feeding practices have been associated with long-term risk of children's weight gain and/or disordered eating, these findings highlight the need for prevention interventions to target knowledge, attitudes, and behaviours of parents of pre-schoolers. Copyright © 2016 Elsevier Ltd. All rights reserved.

Communication with Parents and Body Satisfaction in College Students

ERIC Educational Resources Information Center

Taniguchi, Emiko; Aune, R. Kelly

2013-01-01

Objective: This study examined how communication with parents is related to college students' body satisfaction. Participants and Methods: Participants ("N" = 134; 58 males and 76 females) completed a survey in March 2011 assessing body satisfaction and perceptions of communication with mothers and fathers. Results: Daughters' body…

Does life history shape sexual size dimorphism in anurans? A comparative analysis

PubMed Central

2013-01-01

Background The evolution of sexual size dimorphism (SSD) is likely constrained by life history. Using phylogenetic comparative methods, we examined correlations between SSD among anurans and their life history traits, including egg size, clutch size, mating combat, and parental care behaviour. We used sexual dimorphism index (SDI = Body-sizefemale /Body-sizemale –1) as the measurement for SSD. Body size, life history and phylogenetic data were collected from published literature. Data were analysed at two levels: all anuran species and within individual families. Results Female-biased SSD is the predominant form in anurans. SSD decreases along with the body size increase, following the prediction of Rensch’s rule, but the magnitude of decrease is very small. More importantly, female body size is positively correlated with both fecundity related traits, egg size and clutch size, and SDI is also positively correlated with clutch size, suggesting fecundity advantage may have driven the evolution of female body size and consequently leads to the evolution of female-biased SSD. Furthermore, the presence of parental care, male parental care in particular, is negatively correlated with SDI, indicating that species with parental care tend to have a smaller SDI. A negative correlation between clutch size and parental care further suggests that parental care likely reduces the fecundity selection pressure on female body size. On the other hand, there is a general lack of significant correlation between SDI and the presence of male combat behaviour, which is surprising and contradictory to previous studies. Conclusions We find clear evidence to support the ‘fecundity advantage hypothesis’ and the ‘parental care hypothesis’ in shaping SSD in anurans. Nevertheless, the relationships of both parental care and combat behaviour to the evolution of SSD are complex in anurans and the extreme diversity of life history traits may have masked some potential interesting relationships. Our study represents the most comprehensive study of SSD in anurans to date. PMID:23368708

Indulgent Feeding Style and Children’s Weight Status in Preschool

PubMed Central

Hughes, Sheryl O.; Shewchuk, Richard M.; Baskin, Monica L.; Nicklas, Theresa A.; Qu, Haiyan

2009-01-01

Purpose The primary aim of this study was to examine whether parent affect and child temperament characteristics differ across feeding styles in low-income families, given suggestive evidence. The secondary aim was to examine whether feeding styles were still related to children’s body mass index independent of parent affect, child temperament, and known correlates. Methods Participants in this study were 718 parents of childrens attending Head Start programs across two sites (Texas and Alabama). Parents were categorized into feeding styles of authoritative (n = 118), authoritarian (n = 219), indulgent (n = 240) and uninvolved (n = 141) using a parent-report questionnaire characterizing feeding in a general parenting paradigm. Parents completed questionnaires and measured height and weight was obtained from parents and children. Results Differences were found across feeding styles on parent affect and child temperament characteristics. Indulgent parents reported lower Negative Affect for themselves and lower Negative Affectivity for their children. The indulgent feeding style was significantly associated with higher child body mass index after controlling for parent affect, child temperament, and correlates (ethnicity, child age, parent body mass index). Conclusions The results of this study not only show a robust association between the indulgent feeding style and weight status of low-income preschool childrens, but also suggest how congruence between parent emotional affect and child temperament characteristics may contribute to excess consumption among children of indulgent parents. PMID:18714209

Parental depression, family functioning and obesity among African American children.

PubMed

Davis, Melvin; Young, LaShun; Davis, Sheila P; Moll, George

2008-01-01

Obesity has reached an epidemic level in America (National Center for Health Statistics [NCHS] 1999), and this epidemic is more acute for African Americans than for other groups of Americans. In this study, 44 parent-child dyads completed measurements of height, depression, and body fat composition. In addition, parents completed a demographic questionnaire, and instruments, which measured family functioning, parental psychopathology, child behavior, and cardiovascular risks. Several models emerged for predicting childhood and parental body mass index, parental depression, and child behavioral problems. Findings indicated a role for parental depression in childhood obesity. These findings are discussed in light of Bandura's Social Cognitive Theory, and the family's role in childhood obesity.

Parent/Student Risk and Protective Factors in Understanding Early Adolescent's Body Mass Index

ERIC Educational Resources Information Center

Fitzpatrick, Kevin M.; Willis, Don

2016-01-01

This article's aim is to examine correlates of middle school students' body mass index (BMI). Little research simultaneously has considered both child and parent correlates in predicting child's BMI; we examine the interrelationships between middle school students and their parent's risks and protective factors and their impact on the child's BMI.…

Adolescent Health Care Decision Making: The Law and Public Policy.

ERIC Educational Resources Information Center

Gittler, Josephine; And Others

A large and complicated body of law deals primarily with required parental involvement in health care decisions concerning adolescent children. Addressing that body of legislation, Part 1 of this two-part background paper focuses on a survey of laws requiring parental consent to health services for minors or parental notification of a minor's…

Should Schools Send BMI Report Cards to Parents? A Review of Literature

ERIC Educational Resources Information Center

Henningsen, Alexander; Boros, Piroska; Ingvalson, Kent; Fontana, Fabio E.; Matvienko, Oksana

2015-01-01

A body mass index (BMI) report card is a tool to inform parents about their child's weight status. Body mass index notifications could curb childhood obesity by prompting parents to encourage their children to be more physically active and make better dietary choices, but they could also lower children's self-esteem and increase weight-related…

EARLY IMPACT MELTING AND SPACE EXPOSURE HISTORY OF THE PAT91501 LCHONDRITE

NASA Technical Reports Server (NTRS)

Bogard, Donald D.; Garrison, D. H.; Herzog, G. F.; Xue, S.; Klein, J.; Middleton, R.

2004-01-01

Collisions probably occurred frequently in the early history of the asteroid belt. Their effects, which should be recorded in meteorites, must have included heating and melting along with shock alteration of mineral textures. Some non-chondritic meteorite types e.g., eucrites and IIE and IAB irons - do indeed give evidence of extensive impact heating more than 3.4 Gyr ago. The ordinary chondrites, in contrast, show little evidence of early impact heating. The Ar-Ar and Rb-Sr ages of ordinary chondrites that experienced intense shock are for the most part relatively young, many less than 1.5 Gyr. The numerous L-chondrites with Ar- Ar ages clustering near 0.5 Gy are a well-known example. One of them, the 105-kg Chico Lchondrite, shows the effects of unusually intense heating. It is approximately 60% impact melt and likely formed as a dyke beneath a large crater when the L-chondrite parent body underwent a very large impact approximately 0.5 Gyr ago. In rare instances, older shock dates are indicated for ordinary chondrites. Dixon et al show early impact resetting of Ar-Ar ages of a few LL-chondrites including MIL 99301 at 4.23 0.03 Gyr, but in none of these stones did shock lead to extensive melting. As of 2003, searches for chondritic melts attributable to early shock had turned up only the Shaw L-chondrite, which has an Ar-Ar age of approximately 4.42 Gyr. PAT91501 is an 8.55-kg L-chondrite containing vesicles and metal-troilite nodules. It is a unique, near-total impact melt, unshocked, depleted in siderophile and chalcophile elements, and contains only approximately 10% relic chondritic material. The authors conclude that PAT91501 crystallized rapidly and from a much more homogeneous melt than did Shaw. They suggest that PAT resembles Chico and likely formed as an impact melt vein within an impact crater. To define the history of PAT, we have determined its Ar-39-Ar-40 age and measured several radioactive and stable nuclides produced during its space exposure to cosmic rays.

Evolution of carbonaceous chondrite parent bodies: Insights into cometary nuclei

NASA Technical Reports Server (NTRS)

Mcsween, Harry Y., Jr.

1989-01-01

It is thought that cometary samples will comprise the most primitive materials that are able to be sampled. Although parent body alteration of such samples would not necessarily detract from scientists' interest in them, the possibility exists that modification processes may have affected cometary nuclei. Inferences about the kinds of modifications that might be encountered can be drawn from data on the evolution of carbonaceous chondrite parent bodies. Observations suggest that, of all the classes of chondrites, these meteorites are most applicable to the study of comets. If the proportion of possible internal heat sources such as Al-26 in cometary materials are similar to those in chondrites, and if the time scale of comet accretion was fast enough to permit incorporation of live radionuclides, comets might have had early thermal histories somewhat like those of carbonaceous chondrite parent bodies.

Origin of howardites, diogenites and eucrites - A mass balance constraint

NASA Technical Reports Server (NTRS)

Warren, P. H.

1985-01-01

Two petrogenetic models for the noncumulate-basaltic parts of howardite meteorites are discussed. A mass balance constraint is developed which indicates that more than half of the basaltic components in howardites formed as residual liquids from fractional crystallization of melts that had earlier produced diogentelike pyroxene cumulate components. Other model constriants involving scandium trends, clustering near olivine-pyroxene-plagioclase peritectic, and MgO/(MgO + FeO) ratios are discussed.

Aioun el Atrouss - Evidence for thermal recrystallization of a eurite breccia. [meteoritic mineralogy

NASA Technical Reports Server (NTRS)

Duke, M. B.

1978-01-01

The Aioun el Atrouss meteorite is a breccia consisting largely of angular fragments of green orthopyroxene and containing scattered clasts of basaltic composition (mostly pigeonite and calcic plagioclase). It appears to be a physical mixture of two meteorite types - diogenite (hypersthene achondrite) and eucrite (basaltic achondrite). The results of a mineral analysis are tabulated, and typical pyroxene compositions in orthopyroxene (diogenite), subophitic and granoblastic portions of the meteorite are presented.

Geochemistry and genesis of the angrites

NASA Technical Reports Server (NTRS)

Mittlefehldt, David W.; Lindstrom, Marilyn M.

1990-01-01

The major and trace elements were analyzed in samples of LEW86010, LEW87051, and Angra dos Reis angrites were analyzed using INAA and fused-bead EMP techniques. Results suggest that all three angrites originated on a volatile-depleted (Na-poor) but oxidized parent body or on several bodies. The combination of low Na and high FeO/MnO found in these samples suggests that the extreme Na depletion was caused by parent-body outgassing during differentiation, rather than by nebular processes. It was also found that the refractory-element abundances observed in LEW86010 and LEW87051 are related via olivine control; it is suggested that LEW86010 may be a residual melt from a LEW87051-like precursor or that LEW87051 formed from a LEW86010-like precursor via olivine accumulation. On the other hand, the Angra dos Reis displayed an unusual refractory element pattern suggesting that either the angrite parent body was heterogeneous or that Angra dos Reis was formed on a parent body different from that of the other two angrites.

Encountering the Body at the Site of the Suicide: A Population-Based Survey in Sweden.

PubMed

Omerov, Pernilla; Pettersen, Rossana; Titelman, David; Nyberg, Tommy; Steineck, Gunnar; Dyregrov, Atle; Nyberg, Ullakarin

2017-02-01

Encountering the body of a child who died by suicide at the site of death is believed to be especially harmful for bereaved parents. We investigated the association between encountering the body at the site of the suicide and psychological distress in 666 suicide-bereaved parents. Parents who had encountered their child's body at the site of the suicide (n = 147) did not have a higher risk of nightmares (relative risk [RR] 0.95, 95% confidence interval [CI] 0.67-1.35), intrusive memories (RR 0.97, 95% CI 0.84-1.13), avoidance of thoughts (RR 0.97, 95% CI 0.74-1.27), avoidance of places or things (RR 0.91, 95% CI 0.66-1.25), anxiety (RR 0.93, 95% CI 0.64-1.33), or depression (RR 0.94, 95% CI 0.63-1.42) compared with parents who had not encountered the body (n = 512). Our results suggest that losing a child by suicide is sufficiently disastrous by itself to elicit posttraumatic responses or psychiatric morbidity whether or not the parent has encountered the deceased child at the site of death. © 2016 The American Association of Suicidology.

Workshop on Parent-Body and Nebular Modification of Chondritic Materials

NASA Technical Reports Server (NTRS)

Zolensky, M. E. (Editor); Krot, A. N. (Editor); Scott, E. R. D. (Editor)

1997-01-01

Topics considered include: thermal Metamorphosed Antarctic CM and CI Carbonaceous Chondrites in Japanese Collections, and Transformation Processes of Phyllosilicates; use of Oxygen Isotopes to Constrain the Nebular and Asteroidal Modification of Chondritic Materials; effect of Revised Nebular Water Distribution on Enstatite Chondrite Formation; interstellar Hydroxyls in Meteoritic Chondrules: Implications for the Origin of Water in the Inner Solar System; theoretical Models and Experimental Studies of Gas-Grain Chemistry in the Solar Nebula; chemical Alteration of Chondrules on Parent Bodies; thermal Quenching of Silicate Grains in Protostellar Sources; an Experimental Study of Magnetite Formation in the Solar Nebula; the Kaidun Meteorite: Evidence for Pre- and Postaccretionary Aqueous Alteration; a Transmission Electron Microscope Study of the Matrix Mineralogy of the Leoville CV3 (Reduced-Group) Carbonaceous Chondrite: Nebular and Parent-Body Features; rubidium-Strontium Isotopic Systematic of Chondrules from the Antarctic CV Chondrites Yamato 86751 and Yamato 86009: Additional Evidence for Late Parent-Body Modification; oxygen-Fugacity Indicators in Carbonaceous Chondrites: Parent-Body Alteration or High-Temperature Nebular Oxidation; thermodynamic Modeling of Aqueous Alteration in CV Chondrites; asteroidal Modification of C and O Chondrites: Myths and Models; oxygen Fugacity in the Solar Nebular; and the History of Metal and Sulfides in Chondrites.

Child Disinhibition, Parent Restriction, and Child Body Mass Index in Low-Income Preschool Families

ERIC Educational Resources Information Center

Sparks, Martha A.; Radnitz, Cynthia L.

2013-01-01

Objective: To examine both unique and interactive effects of parent restrictive feeding and child disinhibited eating behavior on child body mass index (BMI) in low-income Latino and African American preschoolers. Methods: The sample included 229 parent-child pairs, the majority of whom were low-income and Latino (57%) or African American (25%).…

Associations of Parental Self-Efficacy with Diet, Physical Activity, Body Composition, and Cardiorespiratory Fitness in Swedish Preschoolers: Results from the MINISTOP Trial

ERIC Educational Resources Information Center

Parekh, Niyati; Henriksson, Pontus; Delisle Nyström, Christine; Silfvernagel, Kristin; Ruiz, Jonatan R.; Ortega, Francisco B.; Pomeroy, Jeremy; Löf, Marie

2018-01-01

Background: High parental self-efficacy (PSE) has been associated with healthy diets and higher levels of physical activity (PA) in children; however, data on PSE in relation to body weight and body composition are scarce. The objective of this study was to investigate associations of PSE with measures of diet, PA, body composition, and physical…

Overweight in children and adolescents associated with TV viewing and parental weight: Project HeartBeat!

PubMed

Steffen, Lyn M; Dai, Shifan; Fulton, Janet E; Labarthe, Darwin R

2009-07-01

Parental obesity and TV viewing are risk factors for childhood obesity. This study assessed the association of children's TV viewing and computer use with body mass and examined whether parental weight status modified the association. Cross-sectional associations of parental weight status, hours of TV viewing and computer use, and children's body composition were studied in a subsample of 526 black and nonblack children, aged 8, 11, and 14 years at baseline, enrolled in Project HeartBeat!, a longitudinal study of cardiovascular disease risk factors, 1991-1995. BMI, fat-free mass (FFM), and percent body fat (PBF) were calculated from children's body composition measured at baseline. Children's TV viewing and computer use habits and parental height and weight were self-reported. Multivariate regression analysis was used in assessing inter-relations of parental weight status and child's TV viewing and computer use habits with BMI, FFM, PBF, and risk for overweight status (BMI > or =85th percentile), adjusting for age, gender, race, and Tanner stage. Children of one or two overweight/obese parents watched an average of 22+/-6 minutes or 30+/-11 minutes more TV per day than children of normal-weight parents, respectively (both p<0.01). In multivariate regression analyses, BMI and PBF increased significantly by 0.42 kg/m(2) and 1.14% (both p<0.001), respectively, for each hour of TV watched among children with overweight parents, but not for those with normal-weight parents (p(interaction)<0.05). Similar results were observed for total screen time. These study findings are consistent with a genetic contribution of parental weight; however, overweight/obese parents may also exhibit behavior patterns that negatively influence children's TV viewing and have an impact on child overweight status. The effect of parental BMI on children's BMI may have both a genetic and an environmental linkage.

Association of parental body mass index before pregnancy on infant growth and body composition: Evidence from a pregnancy cohort study in Malaysia.

PubMed

Zalbahar, Nurzalinda; Jan Mohamed, Hamid Jan B; Loy, See Ling; Najman, Jake; McIntyre, Harold David; Mamun, Abdullah

2016-09-01

Parental body mass index (BMI) is strongly linked with the development of offspring overweight and obesity. However, there are a limited number of studies focusing on the association of parental body mass index before pregnancy on offspring growth and body composition in early life, particularly in developing countries. Data from the University Sains Malaysia (USM) Pregnancy Cohort which consists of 153 mother-offspring pairs were used. Data were collected using interview-administered questionnaires and anthropometric measurements were also obtained. Multiple linear regression and generalised equation estimation (GEE) were used to examine the direction and impact of the association between parental BMI and child growth and body composition (weight for age, height for age, body mass index for age, weight for height and fat mass at age 2m, 6m, and 12m). Potential confounders, including validated measures of maternal diets and physical activity during pregnancy, were considered. Of 153 parents, one-quarter of the mothers and 42.2% of the fathers, respectively, were overweight or obese before pregnancy. A significant association was found between maternal BMI and child's weight for height z-score (WHZ) and body mass index for age z-score (BAZ). Having high pre-pregnancy BMI may increase BMI and WAZ of offspring in early life. Findings from this study emphasise the importance of monitoring maternal weight status, particularly before and during pregnancy and early life of offspring among Malaysians. Copyright © 2015 Asia Oceania Association for the Study of Obesity. Published by Elsevier Ltd. All rights reserved.

Phase equilibrium constraints on angrite petrogenesis

NASA Astrophysics Data System (ADS)

Longhi, John

1999-02-01

Parameterizations of liquidus boundaries and solid solution in the CMAS + Fe system (Shi, 1992) have been employed to depict the liquidus equilibria relevant to the petrogenesis of angrites. Angrites are basaltic achondrites characterized by highly aluminous augite (fassaite), intermediate Mg-Fe olivine, and late-stage CaFe-olivine (kirschsteinite). Two important features of the equilibria on the olivine liquidus surface relevant to angrite petrogenesis are: 1) the presence of a thermal divide on the ol + aug + plag + liq boundary curve, which separates the compositions of source materials that produce low-silica angritic melts that crystallize highly aluminous augite from those that produce higher silica melts with tholeiitic to eucritic crystallization patterns; and 2) the change in the pseudo-invariant point on the low-silica side of the thermal divide from a plagioclase-peritectic involving spinel ( ol + aug + plag + sp + liq) at high to intermediate Mg' (Mg/[Mg + Fe]) to two pseudo-eutectics involving kirschsteinite ( ol + aug + plag + kir + liq and ol + kir + plag + sp + liq) at low Mg'. The fassaitic (aluminous augite) pyroxene composition in Angra Dos Reis (ADOR), the presence of minor green spinel, and the absence of primary kirschsteinite (Prinz et al., 1977) indicate that crystallization of the ADOR parental liquid was governed by the intermediate-Mg' set of equilibria such that, following crystallization of ol + aug + plag, the plagioclase reacted completely at the plagioclase-peritectic with the interstitial liquid, which subsequently crystallized beyond the plagioclase-peritectic onto the ol + aug + sp liquidus boundary curve. The ADOR bulk composition is consistent with trapping ˜10% of the parental liquid in a cumulate with cotectic proportions of fassaite and olivine. Lewis Cliff (LEW)86010 crystallized from a liquid with Mg' similar to that of ADOR, but on the ol + plag cotectic closer to the thermal divide such that the first pyroxene to crystallize had much lower Al content than that of ADOR. In the late stages of crystallization the 86010 residual liquid (and that of LEW87051) encountered the low Mg' set of equilibria involving kirschsteinite. These relationships require either a higher degree of melting for the 86010 parent magma or source region different than ADOR's. These relationships are also consistent with compositionally dependent REE partition coefficients between fassaite and the ADOR liquid being as much as 1.5-2 times higher than those for the 86010 liquid at the onset of pyroxene crystallization. The combination of a trapped liquid component, higher partition coefficients, and smaller degrees of melting help to explain the observation that ADOR, an apparent cumulate, has REE concentrations twice as high as those in 86010 (Mittlefehdlt and Lindstrom, 1990), an apparent chilled liquid. The absence of a strong negative Eu-anomaly in the ADOR parent liquid, however, requires relatively high degrees of partial melting to eliminate plagioclase in the source region (resorption of plagioclase at the peritectic eliminates the Eu-anomaly that develops during crystallization), so ultimately different source regions are required. Progressive iron loss from devolatilized primitive chondrites (Allende, Murchison) produces source regions capable of producing a wide range of melt compositions with angritic to eucritic crystallization behavior. The compositions of carbonaceous and ordinary chondrite provide a similar range of potential source region compositions. However, primitive chondrite(±Fe) source regions that produce angrite-like melts have Mg' that is too low, whereas chondrite(±Fe) sources that have Mg' sufficiently high to yield the Mg' in angrite minerals have too much silica (or orthopyroxene) component to yield angrite-like liquids. No single group of meteorites ± Fe simultaneously satisfies the constraints of Mg' and silica component. However, mixtures of Fe-depleted chondrite plus a low-silica component similar to Ca-Al-rich inclusions (CAIs) can satisfy the constraints. The absence in angrites of 48Ca and 50Ti anomalies, typical of CAIs (Lugmair and Galer, 1992), suggests that the low-silica component was not simply an enrichment of CAIs, but was the result of direct accretion of high-temperature condensate (Grossman, 1972) into sizable, thermally shielded planetesimals. Thus angrites cryptically record mixing of planetesimal-sized heterogeneities in the early solar system.

Metal-rich meteorites from the aubrite parent body

NASA Technical Reports Server (NTRS)

Casanova, I.; Mccoy, T. J.; Keil, K.

1993-01-01

Three metal-rich meteorites - Mt. Egerton, Horse Creek, and LEW 88055 - were studied and it is suggested that they formed in the aubrite parent body. LEW 85369 and 88631 may also have a common origin, but these rocks have not yet been studied in detail. This body was probably heated to about 1600 C by a very strong heat source. While molten, metal agglomerated into sizeable nodules which never segregated efficiently to form a core, but were trapped in the silicate mantle. Different clasts and lithologies in aubrites solidified and cooled under local equilibrium conditions of oxygen fugacity, and with different thermal histories. Impacts mixed clasts from throughout the parent body, creating the typical aubrite breccias.

Contributors to chromium isotope variation of meteorites

NASA Astrophysics Data System (ADS)

Qin, Liping; Alexander, Conel M. O.'D.; Carlson, Richard W.; Horan, Mary F.; Yokoyama, Tetsuya

2010-02-01

We report the results of a comprehensive, high precision survey of the Cr isotopic compositions of primitive chondrites, along with some differentiated meteorites. To ensure complete dissolution of our samples, they were first fused with lithium borate-tetraborate at 1050-1000 °C. Relative to the NIST Cr standard SRM 3112a, carbonaceous chondrites exhibit excesses in 54Cr/ 52Cr from 0.4 to 1.6 ɛ (1 ɛ = 1 part in 10,000), and ordinary chondrites display a common 54Cr/ 52Cr deficit of ˜0.4 ɛ. Analyses of acid-digestion residues of chondrites show that carbonaceous and ordinary chondrites share a common 54Cr-enriched carrier, which is characterized by a large excess in 54Cr/ 52Cr (up to 200 ɛ) associated with a very small deficit in 53Cr/ 52Cr (<2 ɛ). We did not find 54Cr anomalies in either bulk enstatite chondrites or in leachates of their acid-digestion residues. This either requires that the enstatite chondrite parent bodies did not incorporate the 54Cr anomaly carrier phase during their accretion, or the phase was destroyed by parent body metamorphism. Chromium in the terrestrial rocks and lunar samples analyzed here show no deviation from the NIST SRM 3112a Cr standard. The eucrite and Martian meteorites studied exhibit small deficits in 54Cr/ 52Cr. The 54Cr/ 52Cr variations among different meteorite classes suggest that there was a spatial and/or temporal heterogeneity in the distribution of a 54Cr-rich component in the inner Solar System. We confirm the correlated excesses in 54Cr/ 52Cr and 53Cr/ 52Cr for bulk carbonaceous chondrites, but the new data yield a steeper slope (˜6.6) than that reported in Shukolyukov and Lugmair (2006). The correlated excesses may affect the use of the Mn-Cr chronometer in carbonaceous chondrites. We could not confirm the bulk carbonaceous chondrite Mn-Cr isochron reported by Shukolyukov and Lugmair (2006) and Moynier et al. (2007), mostly because we find much smaller total variations in ɛ53Cr (˜0.2). All bulk chondrites have small ɛ53Cr excesses (up to 0.3) relative to the Earth, most likely reflecting the sub-chondritic Mn/Cr ratio of the Earth. The ɛ53Cr variations in chondrites do seem to grossly correlate with Mn/Cr and yield an initial Solar System 53Mn/ 55Mn value of 5.4(±2.4) × 10 -6, corresponding to an absolute age of 4566.4 (±2.2) Ma. Nuclear interactions with cosmic rays result in coupled excesses in ɛ54Cr and ɛ53Cr with a ˜4:1 ratio in phases with high Fe/Cr. These are most dramatically demonstrated in the iron meteorite Carbo, showing excesses in ɛ54Cr of up to 140 ɛ. These new results show that the Mn-Cr chronometer should be used with caution in samples/minerals with high Fe/Cr and long cosmic ray exposure ages.

Association between parental history of diabetes and the incidence of type 2 diabetes mellitus differs according to the sex of the parent and offspring's body weight: A finding from a Japanese worksite-based cohort study.

PubMed

Wang, Chaochen; Yatsuya, Hiroshi; Tamakoshi, Koji; Toyoshima, Hideaki; Wada, Keiko; Li, Yuanying; Hilawe, Esayas Haregot; Uemura, Mayu; Chiang, Chifa; Zhang, Yan; Otsuka, Rei; Ota, Atsuhiko; Hirakawa, Yoshihisa; Aoyama, Atsuko

2015-12-01

To investigate differences in the association of parental history of diabetes with the risk of type 2 diabetes mellitus (T2DM) in the offspring according to the sex of the parent and the offspring's body weight. A prospective cohort study of 4446 middle-aged non-diabetic Japanese men and women were followed in Aichi Prefecture, central Japan, from 2002 to 2011. Subjects were categorized by their self-reported parental history of diabetes ("no parental history," "father only," "mother only," and "both"). The association of parental history of diabetes and incidence in the offspring was examined according to overweight status adjusted for age, sex, birth weight, smoking, alcohol consumption, physical activity, total energy intake, body mass index, and number of metabolic syndrome components. During follow-up (median 8.9 years), 277 subjects developed T2DM. Parental history of diabetes was positively associated with T2DM incidence. However, stratified analysis by overweight status revealed that only maternal history was associated with increased T2DM incidence in non-overweight subjects (hazard ratio=2.35, 95% confidence interval: 1.41-3.91). While in overweight subjects, paternal history was significantly associated with higher T2DM incidence (hazard ratio=1.98, 95% confidence interval: 1.19-3.28). Our results suggest that parental history of diabetes mellitus is associated with the incidence of T2DM in offspring differently according to the sex of the affected parent and the offspring's body weight. Copyright © 2015 Elsevier Inc. All rights reserved.

Preschool-Age Chinese Children's Weight Status: WHO Classification, Parent Ratings, Child/Family Characteristics.

PubMed

Wang, Guang Heng; Tan, Tony Xing; Cheah, Charissa S L

We aimed to compare preschool-age Chinese children's weight status based on the WHO guidelines with parental ratings on their children's body type, and child/family demographic characteristics. The sample included 171 preschool-age children (M=60.5months, SD=6.7; boys: 46.8%) randomly selected from 23 classrooms. Based on BMIs from their height and weight from physical examinations, the children were divided into three groups using the 2006 WHO guidelines: underweight (n=46), normal weight (n=65), and overweight (n=60). Data on the parental ratings of children's current body type, ideal body type and child/family demographic characteristics were collected with surveys. Parents' accurately classified 91.1% of the underweight children, 52.3% of the normal weight children, and 61.7% of the overweight children. In terms of ideal body shape for their children, parents typically wanted their children to have normal weight or to remain underweight. Most of the child and family demographic characteristics were not different across children who were underweight, had normal weight, and were overweight. Because parents tended to underestimate their children's weight status, it is important to increase Chinese parents' knowledge on what constitutes healthy weight, as well as the potential harm of overweight status for children's development. Training healthcare providers in kindergartens and pediatric clinics to work with parents to recognize unhealthy weight status in children is valuable. Copyright © 2016 Elsevier Inc. All rights reserved.

Spectra of Angrites and Possible Parent Bodies

NASA Technical Reports Server (NTRS)

Burbine, T. H.; McCoy, T. J.; Binzel, R. P.

2001-01-01

One meteorite class where very little progress has been made in identifying possible parent bodies is the angrites. We have obtained spectra of two new angrites (D'Orbigny and Sahara 99555). Additional information is contained in the original extended abstract.

Expelled grains from an unseen parent body around AU Microscopii

NASA Astrophysics Data System (ADS)

Sezestre, É.; Augereau, J.-C.; Boccaletti, A.; Thébault, P.

2017-11-01

Context. Recent observations of the edge-on debris disk of AU Mic have revealed asymmetric, fast outward-moving arch-like structures above the disk midplane. Although asymmetries are frequent in debris disks, no model can readily explain the characteristics of these features. Aims: We present a model aiming to reproduce the dynamics of these structures, more specifically their high projected speeds and their apparent position. We test the hypothesis of dust emitted by a point source and then expelled from the system by the strong stellar wind of this young M-type star. In this model we make the assumption that the dust grains follow the same dynamics as the structures, I.e., they are not local density enhancements. Methods: We perform numerical simulations of test particle trajectories to explore the available parameter space, in particular the radial location R0 of the dust producing parent body and the size of the dust grains as parameterized by the value of β (ratio of stellar wind and radiation pressure forces over gravitation). We consider the cases of a static and of an orbiting parent body. Results: We find that for all considered scenarios (static or moving parent body), there is always a set of (R0,β) parameters able to fit the observed features. The common characteristics of these solutions is that they all require a high value of β, of around 6. This means that the star is probably very active, and the grains composing the structures are submicronic in order for observable grains to reach such high β values. We find that the location of the hypothetical parent body is closer in than the planetesimal belt, around 8 ± 2 au (orbiting case) or 28 ± 7 au (static case). A nearly periodic process of dust emission appears, of 2 yr in the orbiting scenarios and 7 yr in the static case. Conclusions: We show that the scenario of sequential dust releases by an unseen point-source parent body is able to explain the radial behavior of the observed structures. We predict the evolution of the structures to help future observations discriminate between the different parent body configurations that have been considered. In the orbiting parent body scenario, we expect new structures to appear on the northwest side of the disk in the coming years.

Predictors of fat stereotypes among 9-year-old girls and their parents.

PubMed

Davison, Kirsten Krahnstoever; Birch, Leann Lipps

2004-01-01

To assess familial links in fat stereotypes and predictors of stereotypes among girls and their parents. Fat stereotypes were assessed using a questionnaire developed for this study. Participants indicated the extent to which they agreed with nine statements about thin people (e.g., thin people are smart) and the same statements about fat people (e.g., fat people are smart). Predictors of fat stereotypes that were examined include weight status (BMI; girls and parents), education (parents), income (parents), self-investment in physical appearance (parents), maladaptive eating attitudes (girls), and parenting practices and peer interactions focused on body shape and weight loss (girls). Girls and parents exhibited fat stereotypes. Fathers who were more educated and had a higher family income were more likely to endorse fat stereotypes, as were mothers and fathers with a high investment in their physical appearance. Although no associations were found between girls' and parents' fat stereotypes, girls were more likely to endorse fat stereotypes when interactions with parents and peers focused on body shape and weight loss. Girls were also more likely to endorse fat stereotypes when they reported higher levels of maladaptive eating attitudes. No associations were found between weight status and fat stereotypes. Although there was no association between girls' and parents' fat stereotypes, girls were more likely to express negative attitudes about obesity and obese persons when parenting practices and interactions with peers promoted a lean body type, suggesting that there may be an implicit link between the lean ideal and fat stereotypes.

Parental education and family income affect birthweight, early longitudinal growth and body mass index development differently.

PubMed

Bramsved, Rebecka; Regber, Susann; Novak, Daniel; Mehlig, Kirsten; Lissner, Lauren; Mårild, Staffan

2018-01-07

This study investigated the effects of two parental socio-economic characteristics, education and income, on growth and risk of obesity in children from birth to 8 years of age. Longitudinal growth data and national register-based information on socio-economic characteristics were available for 3,030 Swedish children. The development of body mass index (BMI) and height was compared in groups dichotomised by parental education and income. Low parental education was associated with a higher BMI from 4 years of age, independent of income, immigrant background, maternal BMI and smoking during pregnancy. Low family income was associated with a lower birthweight, but did not independently predict BMI development. At 8 years of age, children from less educated families had a three times higher risk of obesity, independent of parental income. Children whose parents had fewer years of education but high income had significantly higher height than all other children. Parental education protected against childhood obesity, even after adjusting for income and other important parental characteristics. Income-related differences in height, despite similar BMIs, raise questions about body composition and metabolic risk profiles. The dominant role of education underscores the value of health literacy initiatives for the parents of young children. ©2018 Foundation Acta Paediatrica. Published by John Wiley & Sons Ltd.

Composition of Rheasilvia Basin on Asteroid Vesta

NASA Technical Reports Server (NTRS)

Ammannito, Eleonora; DeSanctis, Maria Christina; Capaccioni, Fabrizio; Capria, Maria Teresa; Combe, Jean Philippe; Frigeri, Alessandro; Jaumann, Ralf; Longobardo, Andrea; Marchi, Somone; McCord, Thomas B.;

Two-year-olds' understanding of self-symbols.

PubMed

Herold, Katherine; Akhtar, Nameera

2014-09-01

This study investigated 48 2.5-year-olds' ability to map from their own body to a two-dimensional self-representation and also examined relations between parents' talk about body representations and their children's understanding of self-symbols. Children participated in two dual-representation tasks in which they were asked to match body parts between a symbol and its referent. In one task, they used a self-symbol and in the other they used a symbol for a doll. Participants were also read a book about body parts by a parent. As a group, children found the self-symbol task more difficult than the doll-task; however, those whose parents explicitly pointed out the relation between their children's bodies and the symbols in the book performed better on the self-symbol task. The findings demonstrate that 2-year-old children have difficulty comprehending a self-symbol, even when it is two-dimensional and approximately the same size as them, and suggest that parents' talk about self-symbols may facilitate their understanding. © 2014 The British Psychological Society.

The 2014 KCG Meteor Outburst: Clues to a Parent Body

NASA Technical Reports Server (NTRS)

Moorhead, Althea V.; Brown, Peter G.; Spurny, Pavel; Cooke, William J.

2015-01-01

The Kappa Cygnid (KCG) meteor shower exhibited unusually high activity in 2014, producing ten times the typical number of meteors. The shower was detected in both radar and optical systems and meteoroids associated with the outburst spanned at least five decades in mass. In total, the Canadian Meteor Orbit Radar, European Network, and NASA All Sky and Southern Ontario Meteor Network produced thousands of KCG meteor trajectories. Using these data, we have undertaken a new and improved characterization of the dynamics of this little-studied, variable meteor shower. The Cygnids have a di use radiant and a significant spread in orbital characteristics, with multiple resonances appearing to play a role in the shower dynamics. We conducted a new search for parent bodies and found that several known asteroids are orbitally similar to the KCGs. N-body simulations show that the two best parent body candidates readily transfer meteoroids to the Earth in recent centuries, but neither produces an exact match to the KCG radiant, velocity, and solar longitude. We nevertheless identify asteroid 2001 MG1 as a promising parent body candidate.

Cosmic-ray exposure ages of the ordinary chondrites and their significance for parent body stratigraphy

NASA Technical Reports Server (NTRS)

Crabb, J.; Schultz, L.

1981-01-01

Improved exposure ages are derived for 201 H, 203 L, and 38 LL chondrites in an effort to understand the characteristics of the chondrite parent body. The Ne-21 exposure ages were calculated from literature values taking into account shielding differences, a trapped component and radiogenic He. The exposure age distributions show clear peaks at 4.5 and 20 million years for the H chondrites, while the Ls and LLs appear more as a continuous series of intermediate peaks which may be modeled by at least six peaks between 1 and 35 million years in the case of L chondrites. The observations that every petrological type occurs in each large peak and contain solar wind gases suggest that the parent bodies have been fragmented and reassembled into a megabreccia. The H meteorites are proposed to represent the surface layer of a body with a substantial, active regolith as indicated by the relatively high abundances of solar gases. The L chondrites, on the other hand, are attributed to a parent body that was fragmented by collision about 500 million years ago.

Parental and Peer Factors Associated with Body Image Discrepancy among Fifth-Grade Boys and Girls

PubMed Central

Wentzel, Kathryn; Elliott, Marc N.; Dittus, Patricia J.; Kanouse, David E.; Wallander, Jan L.; Pasch, Keryn E.; Franzini, Luisa; Taylor, Wendell C.; Qureshi, Tariq; Franklin, Frank A.; Schuster, Mark A.

2015-01-01

Many young adolescents are dissatisfied with their body due to a discrepancy between their ideal and actual body size, which can lead to weight cycling, eating disorders, depression, and obesity. The current study examined the associations of parental and peer factors with fifth-graders’ body image discrepancy, physical self-worth as a mediator between parental and peer factors and body image discrepancy, and how these associations vary by child’s sex. Body image discrepancy was defined as the difference between young adolescents’ self-perceived body size and the size they believe a person their age should be. Data for this study came from Healthy Passages, which surveyed 5,147 fifth graders (51 % females; 34 % African American, 35 % Latino, 24 % White, and 6 % other) and their primary caregivers from the United States. Path analyses were conducted separately for boys and girls. The findings for boys suggest father nurturance and getting along with peers are related negatively to body image discrepancy; however, for girls, fear of negative evaluation by peers is related positively to body image discrepancy. For both boys and girls, getting along with peers and fear of negative evaluation by peers are related directly to physical self-worth. In addition, mother nurturance is related positively to physical self-worth for girls, and father nurturance is related positively to physical self-worth for boys. In turn, physical self-worth, for both boys and girls, is related negatively to body image discrepancy. The findings highlight the potential of parental and peer factors to reduce fifth graders’ body image discrepancy. PMID:23334988

Lithologies Making Up CM Carbonaceous Chondrites and Their Link to Space Exposure Ages

NASA Technical Reports Server (NTRS)

Gregory, Timothy; Zolensky, Michael E.; Trieman, Alan; Berger, Eve; Le, Loan; Fagan, Amy; Takenouchi, Atsushi; Velbel, Michael A.; Nishiizumi, Kunihiko

2015-01-01

Chondrite parent bodies are among the first large bodies to have formed in the early Solar System, and have since remained almost chemically unchanged having not grown large enough or quickly enough to undergo differentiation. Their major nonvolatile elements bear a close resemblance to the solar photosphere. Previous work has concluded that CM chondrites fall into at least four distinct space exposure age groups (0.1 Ma, 0.2 Ma, 0.6 Ma and >2.0 Ma), but the meaning of these groupings is unclear. It is possible that these meteorites came from different parent bodies which broke up at different times, or instead came from the same parent body which underwent multiple break-up events, or a combination of these scenarios.

Lithologies Making Up CM Carbonaceous Chondrites and Their Link to Space Exposure Ages

NASA Technical Reports Server (NTRS)

Gregory, Timothy; Zolensky, Michael E.; Trieman, Alan; Berger, Eve; Le, Loan; Fagan, Amy; Takenouchi, Atsushi; Velbel, Michael A.; Nishiizumi, Kuni

2015-01-01

Chondrite parent bodies are among the first large bodies to have formed in the early Solar System, and have since remained almost chemically unchanged having not grown large enough or quickly enough to undergo differentiation. Their major nonvolatile elements bear a close resemblance to the solar photosphere. Previous work has concluded that CM chondrites fall into at least four distinct space exposure age groups (0.1 megaannus, 0.2 megaannus, 0.6 megaannus and 2.0 megaannus), but the meaning of these groupings is unclear. It is possible that these meteorites came from different parent bodies which broke up at different times, or instead came from the same parent body which underwent multiple break-up events, or a combination of these scenarios.

Identifying Asteroidal Parent Bodies of the Meteorites: The Last Lap

NASA Technical Reports Server (NTRS)

Gaffey, M. J.

2000-01-01

Spectral studies of asteroids and dynamical models have converged to yield, at last, a clear view of asteroid-meteorite linkages. Plausible parent bodies for most meteorite types have either been identified or it has become evident where to search for them.

Parents' education and child body weight in France: The trajectory of the gradient in the early years.

PubMed

Apouey, Bénédicte H; Geoffard, Pierre-Yves

2016-03-01

This paper explores the relationship between parental education and offspring body weight in France. Using two large datasets spanning the 1991-2010 period, we examine the existence of inequalities in maternal and paternal education and reported child body weight measures, as well as their evolution across childhood. Our empirical specification is flexible and allows this evolution to be non-monotonic. Significant inequalities are observed for both parents' education--maternal (respectively paternal) high education is associated with a 7.20 (resp. 7.10) percentage points decrease in the probability that the child is reported to be overweight or obese, on average for children of all ages. The gradient with respect to parents' education follows an inverted U-shape across childhood, meaning that the association between parental education and child body weight widens from birth to age 8, and narrows afterward. Specifically, maternal high education is correlated with a 5.30 percentage points decrease in the probability that the child is reported to be overweight or obese at age 2, but a 9.62 percentage points decrease at age 8, and a 1.25 percentage point decrease at age 17. The figures for paternal high education are respectively 5.87, 9.11, and 4.52. This pattern seems robust, since it is found in the two datasets, when alternative variables for parental education and reported child body weight are employed, and when controls for potential confounding factors are included. The findings for the trajectory of the income gradient corroborate those of the education gradient. The results may be explained by an equalization in actual body weight across socioeconomic groups during youth, or by changes in reporting styles of height and weight. Copyright © 2015 Elsevier B.V. All rights reserved.

The mediating effects of perceived parental teasing on relations of body mass index to depression and self-perception of physical appearance and global self-worth in children.

PubMed

Bang, Kyung-Sook; Chae, Sun-Mi; Hyun, Myung-Sun; Nam, Hye Kyung; Kim, Ji-Soo; Park, Kwang-Hee

2012-12-01

To report a correlational study of the relation of body mass index to children's perceptions of physical appearance and global self-worth and depression, as mediated by their perceptions of parental teasing. The relation between depression and self-perception in children with obesity has been reported. Recently, parental factors were found to be related to childhood obesity. Little is known about the effects of perceived parental teasing on depression and self-perception in children. A descriptive correlational research design was used. Data were collected from 455 children in the fifth and sixth grades in four provinces of South Korea using self-report questionnaires for measuring self-perception of physical appearance and global self-worth, depression and perceived parental teasing between October-December in 2009. The children's weight and height information from school health records was used. Multiple regression analysis and the Sobel test were used to identify the mediating effect of perceived parental teasing. Among the children, 20% were overweight or obese. Although children with obesity did not differ in the level of depression from their normal weight counterparts, they demonstrated lower perceived physical appearance and higher perceived parental teasing. The mediating effects of perceived parental teasing were found for the relations between body mass index and self-perception of physical appearance and global self-worth, and body mass index and depression, respectively. Obese children at risk of parental teasing should be identified to prevent their psychological problems. A well-designed intervention study is necessary to examine the effects of psycho-emotional interventions for obese children. © 2012 Blackwell Publishing Ltd.

The accretion and impact history of the ordinary chondrite parent bodies

NASA Astrophysics Data System (ADS)

Blackburn, Terrence; Alexander, Conel M. O'D.; Carlson, Richard; Elkins-Tanton, Linda T.

2017-03-01

A working timeline for the history of ordinary chondrites includes chondrule formation as early as 0-2 Ma after our Solar System's earliest forming solids (CAIs), followed by rapid accretion into undifferentiated planetesimals that were heated internally by 26Al decay and cooled over a period of tens of millions of years. There remains conflict, however, between metallographic cooling rate (Ni-metal) and radioisotopic thermochronometric data over the sizes and lifetimes of the chondrite parent bodies, as well as the timing of impact related disruptions. The importance of establishing the timing of parent body disruption is heightened by the use of meteorites as recorders of asteroid belt wide disruption events and their use to interpret Solar System dynamical models. Here we attempt to resolve these records by contributing new 207Pb-206Pb data obtained on phosphates isolated from nine previously unstudied ordinary chondrites. These new results, along with previously published Pb-phosphate, Ni-metal and thermometry data, are interpreted with a series of numerical models designed to simulate the thermal evolution for a chondrite parent body that either remains intact or is disrupted by impact prior to forming smaller unsorted "rubble piles". Our thermal model and previously published thermometry data limit accretion time to 2.05-2.25 Ma after CAIs. Measured Pb-phosphate data place minimum estimates on parent body diameters of ∼260-280 km for both the L and H chondrite parent bodies. They also consistently show that petrologic Type 6 (highest thermal metamorphism) chondrites from both the H and L bodies have younger ages and, therefore, cooled more slowly than Type 5 (lesser metamorphism) chondrites. This is interpreted as evidence for Type 5 chondrite origination from shallower depths than Type 6 chondrites within initially concentrically zoned bodies. This contrasts metallographic cooling rate data that are inconsistent with such a simple onion shell scenario. One model that can reconcile these two data sets takes into account subtle differences in temperature to which each system responds. This working model requires that disruption occur early enough such that the Ni-metal system can record the cooling rate associated with a rubble pile (<70 Ma), yet late enough that the Pb-phosphate system can record an onion shell structure (>30 Ma). For this 30-70 Ma timeline, reaccretion into smaller rubble piles will ensure that the originally deeply buried and hot Type 6 samples will always cool faster as a result of disruption, yielding nearly uniform ages that record the time of parent body disruption. This is consistent with the available Pb-phosphate data, where all but one Type 6 chondrite (H, n = 3; L, n = 4) yields a cooling age within a narrow 4505 ± 5 Ma timeframe. These data collectively imply that both the H and L chondrite parent bodies were catastrophically disrupted at ∼60 Ma. In addition, combined Ni-metal and Pb-phosphate models confirm that a subset of Type 4 chondrites record early rapid cooling likely associated with erosional impacting of the H and L parent bodies on ∼5 Ma timescales.

Enstatite chondrites and enstatite achondrites (aubrites) were not derived from the same parent body

NASA Technical Reports Server (NTRS)

Brett, Robin; Keil, Klaus

1986-01-01

Enstatite achondrites (aubrites) were not derived from known enstatite chondrites by melting and fractionation on one and the same parent body, for these and other reasons: (1) There is no satisfactory mechanism for fractionating metal plus troilite in enstatite chondrites to form these phases in different proportions and with different Ti contents in aubrites. (2) Many enstatite chondrites and aubrites are regolith or fragmental breccias, but clasts of one within the other have not been found. (3) Cosmic ray exposure ages of the two groups are difficult to explain if they are from the same parent body, but are easy to explain if they are from different parent bodies. Siderophile element abundances in metal from the Mt. Egerton meteorite, which consists of enstatite and metallic Fe, Ni, preclude it from being a complementary differentiate of the aubrites. Rather, it appears that Mt. Egerton was formed from the same source material as enstatite chondrites, but the components were mixed in different proportions.

Enstatite chondrites and enstatite achondrites (aubrites) were not derived from the same parent body

USGS Publications Warehouse

Brett, R.; Keil, Klaus

1986-01-01

Enstatite achondrites (aubrites) were not derived from known enstatite chondrites by melting and fractionation on one and the same parent body, for these and other reasons: (1) There is no satisfactory mechanism for fractionating metal plus troilite in enstatite chondrites to form these phases in different proportions and with different Ti contents in aubrites. (2) Many enstatite chondrites and aubrites are regolith or fragmental breccias, but clasts of one within the other have not been found. (3) Cosmic ray exposure ages of the two groups are difficult to explain if they are from the same parent body, but are easy to explain if they are from different parent bodies. Siderophile element abundances in metal from the Mt. Egerton meteorite, which consists of enstatite and metallic Fe,Ni, preclude it from being a complementary differentiate of the aubrites. Rather, it appears that Mt. Egerton was formed from the same source material as enstatite chondrites, but the components were mixed in different proportions. ?? 1986.

Mid-IR Spectra of HED Meteorites and Synthetic Pyroxenes: Reststrahlen Features (9-12 micron)

NASA Technical Reports Server (NTRS)

Lim, Lucy F.; Emery, Joshua P.; Moskovitz, Nicholas A.

2010-01-01

In an earlier study. Hamilton (2000) mapped the behavior of the 9-12 micron reststrahlen structures with composition in a suite of primarily natural terrestrial pyroxenes. Here we examine the same set of reststrahlen features in the spectra of diogenites and eucrites and place them in the context of the terrestrial samples and of a suite of well-characterized synthetic pyroxenes. The results will be useful to the interpretation of mid-IR spectra of 4 Vesta and other basaltic asteroids.

Water and the thermal evolution of carbonaceous chondrite parent bodies

NASA Technical Reports Server (NTRS)

Grimm, Robert E.; Mcsween, Harry Y., Jr.

1989-01-01

Two hypotheses are proposed for the aqueous alteration of carbonaceous chondrites within their parent bodies, in which respectively the alteration occurs (1) throughout the parent body interior, or (2) in a postaccretional surface regolith; both models assume an initially homogeneous mixture of ice and rock that is heated through the decay of Al-26. Water is seen to exert a powerful influence on chondrite evolution through its role of thermal buffer, permitting substitution of a low temperature aqueous alteration for high temperature recrystallization. It is quantitatively demonstrated that liquid water may be introduced by either hydrothermal circulation, vapor diffusion from below, or venting due to fracture.

Weight-Related Health Behaviors and Body Mass: Associations between Young Adults and Their Parents, Moderated by Parental Authority

ERIC Educational Resources Information Center

Niemeier, Brandi S.; Hektner, Joel M.

2012-01-01

Background: Parents' behaviors could contribute to the development of their children's weight-related health behaviors. Purpose: Relationships of young adults' (N = 151) and their parents' weight-related behaviors were examined along with parental authority styles. Methods: Questionnaires were completed by young adults and their parents.…

Compositional Homogeneity of CM Parent Bodies

NASA Astrophysics Data System (ADS)

Vernazza, P.; Marsset, M.; Beck, P.; Binzel, R. P.; Birlan, M.; Cloutis, E. A.; DeMeo, F. E.; Dumas, C.; Hiroi, T.

2016-09-01

CM chondrites are the most common type of hydrated meteorites, making up ˜1.5% of all falls. Whereas most CM chondrites experienced only low-temperature (˜0°C-120°C) aqueous alteration, the existence of a small fraction of CM chondrites that suffered both hydration and heating complicates our understanding of the early thermal evolution of the CM parent body(ies). Here, we provide new constraints on the collisional and thermal history of CM-like bodies from a comparison between newly acquired spectral measurements of main-belt Ch/Cgh-type asteroids (70 objects) and existing laboratory spectral measurements of CM chondrites. It first appears that the spectral variation observed among CM-like bodies is essentially due to variations in the average regolith grain size. Second, the spectral properties of the vast majority (unheated) of CM chondrites resemble both the surfaces and the interiors of CM-like bodies, implying a “low” temperature (<300°C) thermal evolution of the CM parent body(ies). It follows that an impact origin is the likely explanation for the existence of heated CM chondrites. Finally, similarly to S-type asteroids and (2) Pallas, the surfaces of large (D > 100 km)—supposedly primordial—Ch/Cgh-type main-belt asteroids likely expose the interiors of the primordial CM parent bodies, a possible consequence of impacts by small asteroids (D < 10 km) in the early solar system.

Redistribution of Sr and rare earth elements in the matrices of CV3 carbonaceous chondrites during aqueous alteration in their parent body

NASA Astrophysics Data System (ADS)

Jogo, Kaori; Ito, Motoo; Nakamura, Tomoki; Kobayashi, Sachio; Lee, Jong Ik

2018-03-01

We measured the abundances of Sr and rare earth elements (REEs) in the matrices of five CV3 carbonaceous chondrites: Meteorite Hills (MET) 00430, MET 01070, La Paz ice field (LAP) 02206, Asuka (A) 881317 and Roberts Massif (RBT) 04143. In the MET 00430 and MET 01074 matrices, the Sr/CI and light REE (LREE, La-Nd)/CI ratios positively correlate with the amounts of Ca-rich secondary minerals, which formed during aqueous alteration in the CV3 chondrite parent body. In contrast, in the LAP 02206 and RBT 04143 matrices, although the Sr/CI ratios correlate with the amounts of Ca-rich secondary minerals, the LREE/CI ratios vary independently from the amounts of any secondary minerals. This suggests that the LREE/CI ratios in these matrices were produced prior to the parent body alteration, probably in the solar nebula. The LREE/CI ratios of the LAP 02206 and RBT 04143 matrices reveal the mixing process of matrix minerals prior to the accretion of the CV3 chondrite parent body. The mixing degrees of matrix minerals might be different between these two matrices. Because solid materials would be mixed over time according to the radial diffusion model of a turbulent disk, the matrix minerals consisting of LAP 02206 and RBT 04143 matrices might be incorporated into their parent body with different timing.

Near-infrared spectroscopy of 3:1 Kirkwood Gap asteroids III

NASA Astrophysics Data System (ADS)

Fieber-Beyer, Sherry K.; Gaffey, Michael J.

2015-09-01

The research is an integrated effort beginning with telescopic observations and extending through detailed mineralogical characterizations to provide constraints on the composition and meteorite affinities of a subset of fourteen asteroids in/near the 3:1 Kirkwood Gap. Eight asteroids were identified as having either one or two absorption features, while six were deemed featureless. The compositional analysis of Asteroids (355) Gabriella and (1447) Utra reveal Fs and Fa values which are consistent with values for the L-type ordinary chondrites (Fs19-22 and Fa22-26). The location of these two bodies with respect to each other and to the previously identified L-chondrite parent body Asteroid (1722) Goffin, suggests a small L-chondrite genetic family. These results support the model that the L-chondrites come from an asteroid family rather than from a single object. Asteroids (1368) Numidia, (1587) Kahrstadt, (1854) Skvortsov, (2497) Kulikovskij, and (5676) Voltaire were analyzed and determined to have "basaltic" silicate mineralogies similar to those of the HED (howardite-eucrite-diogenite) meteorite group. In particular, we found that the compositions of (1368), (1587) and (1854) are consistent with olivine-orthopyroxenitic diogenites, while (2497) and (5676)'s compositions are consistent with harzburgitic diogenites. The Band I and Band II absorption feature depths are much shallower than seen in diogenite spectra, typically ∼70% depth (Burbine, T.H. et al. [2000]. Forging asteroid-meteorite relationships through reflectance spectroscopy. Lunar Planet. Sci. XXXI. Abstract 1844). The nature of the weak features seen in the asteroid spectra when compared to measured band depths of in situ diogenite samples indicate an additional mechanism(s) acting to weaken the features, most likely space weathering. The aforementioned five asteroids are plausible sources for the olivine-orthopyroxenitic diogenites and harzburgitic diogenites, and very well may be fragments of Vesta. Asteroid (46) Hestia is an interesting object whose surface minerals may be consistent with a CR2 chondrite; however, the unique spectrum deserves further study in the future. Featureless Asteroids (248) Lameia, (1960) Guisan, (3345) Tarkovskij and (6212) 1993 MS1 surface materials are likely organic assemblages consistent with the Type 1 or 2 carbonaceous chondrite meteorite class; however specific terrestrial meteorite analog could not be identified. The spectra of Asteroids (3228) Pire and (3999) Aristarchus are consistent with each other and have been assigned to the Eulalia by Walsh et al. (Walsh, K.J. et al. [2013]. Icarus 225, 283-297). Spectrally they are similar to (495) in terms of blue-slope and albedo (Fieber-Beyer, S.K., et al. [2012]. Icarus 221, 593-602), thus increasing our confidence the three bodies are truly related dynamically and genetically. By extrapolation and due to their location adjacent to the 3:1 Kirkwood Gap, (3228) and (3999) are plausible sources of the CV3OXB carbonaceous chondrites.

The influence of parental encouragement and caring about healthy eating on children's diet quality and body weights.

PubMed

Faught, Erin; Vander Ploeg, Kerry; Chu, Yen Li; Storey, Kate; Veugelers, Paul J

2016-04-01

In order to mitigate childhood obesity, evidence on what influences children's health behaviours is needed to inform new health promotion strategies. The present study investigated the association between parental practices and their child's diet and body weight status. Grade 5 students and their parents completed health surveys. Parents were asked how much they 'encourage their child to eat healthy foods' and how much they 'personally care about healthy eating'. Children's diet quality and vegetable and fruit intake were assessed using an FFQ. Children's heights and weights were measured to determine body weight status. Mixed-effects regression models were used to determine the influence of parental responses on the outcomes of interest. Elementary schools across the province of Alberta, Canada. Grade 5 students (aged 10 and 11 years; n 8388) and their parent(s). Most parents reported caring about healthy eating and encouraging their child to eat healthy foods at least quite a lot. Children whose parents who cared or encouraged 'very much' compared with 'quite a lot' were more likely have better diet quality and were less likely to be overweight. Children whose parents both cared and encouraged 'very much' compared with 'quite a lot' scored an average of 2·06 points higher on the diet quality index (β=2·06; 95 % CI 1·45, 2·66). Health promotion strategies that aim for a high level of parental interest and encouragement of their children to eat healthy foods may improve diet quality and prevent overweight among children.

Overweight and obesity among Malay primary school children in Kota Bharu, Kelantan: parental beliefs, attitudes and child feeding practices.

PubMed

Wan, Abdul Manan W M; Norazawati, A K; Lee, Y Y

2012-04-01

The increasing prevalence of overweight and obesity among children has become a major public health problem in Malaysia. Parents play an important role in child feeding especially among younger children. A study was conducted to evaluate the beliefs, attitudes and practices in child feeding among parents of normal weight, as well as overweight and obese primary school children in Kelantan using the Child Feeding Questionnaire (CFQ). This cross-sectional study was carried out on 175 Malay children from three schools in Kota Bharu district in Kelantan. This study showed that 13.1% of the children were overweight and obese. Scores for perceived parent weight (p < 0.05) and perceived child weight (p < 0.001) were significantly higher among parents of overweight and obese children compared to parents of children with normal body weight. However, the score for pressure to eat among parents of overweight and obese children was significantly lower (p < 0.05) than parents of normal weight children. The perceived child weight (r = 0.468, p < 0.01), perceived parental weight (r = 0.190, p < 0.05) and food restriction (r = 0.179, p < 0.05) factors were found to be positively correlated with children's body mass index (BMI), whereas pressure to eat factor (r = -0.355, p < 0.01) was negatively correlated with children's body mass index (BMI). The findings showed that parental feeding practices were linked to children's weight status and childhood obesity. Therefore parents should be given education and guidance on appropriate child feeding practices to maintain their child's nutritional status on a healthy weight range.

Parent-Child Resemblance in Weight Status and Its Correlates in the United States

PubMed Central

Liang, Lan; Wang, Youfa

2013-01-01

Background Few studies have examined parent-child resemblance in body weight status using nationally representative data for the US. Design We analyzed Body Mass Index (BMI), weight status, and related correlates for 4,846 boys, 4,725 girls, and their parents based on US nationally representative data from the 2006 and 2007 Medical Expenditure Panel Survey (MEPS). Pearson partial correlation coefficients, percent agreement, weighted kappa coefficients, and binary and multinomial logistic regression were used to examine parent-child resemblance, adjusted for complex sampling design. Results Pearson partial correlation coefficients between parent and child’s BMI measures were 0.15 for father-son pairs, 0.17 for father-daughter pairs, 0.20 for mother-son pairs, and 0.23 for mother-daughter pairs. The weighted kappa coefficients between BMI quintiles of parent and child ranged from −0.02 to 0.25. Odds ratio analyses found children were 2.1 (95% confidence interval (CI): 1.6, 2.8) times more likely to be obese if only their father was obese, 1.9 (95% CI: 1.5, 2.4) times more likely if only their mother was obese, and 3.2 (95% CI: 2.5, 4.2) times more likely if both parents were obese. Conclusions Parent-child resemblance in BMI appears weak and may vary across parent-child dyad types in the US population. However, parental obesity status is associated with children’s obesity status. Use of different measures of parent-child resemblance in body weight status can lead to different conclusions. PMID:23762352

Thermal evolution of a partially differentiated H chondrite parent body

NASA Astrophysics Data System (ADS)

Abrahams, J. N. H.; Bryson, J. F. J.; Weiss, B. P.; Nimmo, F.

2016-12-01

It has traditionally been assumed that planetesimals either melted entirely or remained completely undifferentiated as they accreted. The unmelted textures and cooling histories of chondrites have been used to argue that these meteorites originated from bodies that never differentiated. However, paleomagnetic measurements indicate that some chondrites (e.g., the H chondrite Portales Valley and several CV chondrites) were magnetized by a core dynamo magnetic field, implying that their parent bodies were partially differentiated. It has been unclear, however, whether planetesimal histories consistent with dynamo production can also be consistent with the diversity of chondrite cooling rates and ages. To address this, we modeled the thermal evolution of the H chondrite parent body, considering a variety of accretion histories and parent body radii. We considered partial differentiation using two-stage accretion involving the initial formation and differentiation of a small body, followed by the later addition of low thermal conductivity chondritic material that remains mostly unmelted. We were able to reproduce the measured thermal evolution of multiple H chondrites for a range of parent body parameters, including initial radii from 70-150 km, chondritic layer thicknesses from 50 km to over 100 km, and second stage accretion times of 2.5-3 Myr after solar system formation. Our predicted rates of core cooling and crystallization are consistent with dynamo generation by compositional convection beginning 60-200 Myr after solar system formation and lasting for at least tens of millions of years. This is consistent with magnetic studies of Portales Valley [Bryson et al., this meeting]. In summary, we find that thermal models of partial differentiation are consistent the radiometric ages, magnetization, and cooling rates of a diversity H chondrites.

Between Concealing and Revealing Intersexed Bodies: Parental Strategies.

PubMed

Danon, Limor Meoded; Krämer, Anike

2017-08-01

Parents of intersex children are perceived in many studies as hopeless, highly dependent on the medical system, and as gate keepers of normative gendered bodies. In this article, we challenge these perceptions and argue that parents of intersex children are problematically positioned between their children's needs for care and well-being and the socialmedical forces that aim to "normalize" them. Their in-between position leads them to establish different parental strategies within and outside of traditional sex/gender norms. We focus on three intertwined parental strategy frameworks: bodily dialogue, sex/gender framing, and concealing/revealing practices, and describe how, in each of these strategic frameworks, the parents maneuver, act in accordance with or against, react to, and challenge the medical system, social interactions, and the sex/gender paradigm. This is a comparative study based on narrative interviews with 22 parents of intersex children in Germany and Israel.

Parental Bonds, Attachment Anxiety, Media Susceptibility, and Body Dissatisfaction: A Mediation Model

ERIC Educational Resources Information Center

Patton, Sarah C.; Beaujean, A. Alexander; Benedict, Helen E.

2014-01-01

The developmental trajectory of body image dissatisfaction is unclear. Researchers have investigated sociocultural and developmental risk factors; however, the literature needs an integrative etiological model. In 2009, Cheng and Mallinckrodt proposed a dual mediation model, positing that poor-quality parental bonds, via the mechanisms of…

A Petrologic Study of the IAB Iron Meteorites: Constraints on the Formation of the IAB-Winonaite Parent Body

NASA Technical Reports Server (NTRS)

Benedix, G. K.; McCoy, T. J.; Keil, K.; Love, S. G.

1998-01-01

We have studied IAB iron meteorites and their silicate-bearing inclusions to elucidate the origin of their parent body. We have divided IAB irons into five categories which best describe the inclusions and other properties of the irons.

Does Parental Divorce Moderate the Heritability of Body Dissatisfaction? An Extension of Previous Gene-Environment Interaction Effects

PubMed Central

O’Connor, Shannon M.; Klump, Kelly L.; VanHuysse, Jessica L.; McGue, Matt; Iacono, William

2015-01-01

Objective Previous research suggests that parental divorce moderates genetic influences on body dissatisfaction. Specifically, the heritability of body dissatisfaction is higher in children of divorced versus intact families, suggesting possible gene-environment interaction effects. However, prior research is limited to a single, self-report measure of body dissatisfaction. The primary aim of the present study was to examine whether these findings extend to a different dimension of body dissatisfaction, body image perceptions. Method Participants were 1,534 female twins from the Minnesota Twin Family Study, ages 16–20 years. The Body Rating Scale (BRS) was used to assess body image perceptions. Results Although BRS scores were heritable in twins from divorced and intact families, the heritability estimates in the divorced group were not significantly greater than estimates in the intact group. However, there were differences in nonshared environmental effects, where the magnitude of these environmental influences was larger in the divorced as compared to the intact families. Discussion Different dimensions of body dissatisfaction (i.e., negative self-evaluation versus body image perceptions) may interact with environmental risk, such as parental divorce, in discrete ways. Future research should examine this possibility and explore differential gene x environment interactions using diverse measures. PMID:26314278

Does parental divorce moderate the heritability of body dissatisfaction? An extension of previous gene-environment interaction effects.

PubMed

O'Connor, Shannon M; Klump, Kelly L; VanHuysse, Jessica L; McGue, Matt; Iacono, William

2016-02-01

Previous research suggests that parental divorce moderates genetic influences on body dissatisfaction. Specifically, the heritability of body dissatisfaction is higher in children of divorced versus intact families, suggesting possible gene-environment interaction effects. However, prior research is limited to a single, self-reported measure of body dissatisfaction. The primary aim of this study was to examine whether these findings extend to a different dimension of body dissatisfaction: body image perceptions. Participants were 1,534 female twins from the Minnesota Twin Family Study, aged 16-20 years. The Body Rating Scale (BRS) was used to assess body image perceptions. Although BRS scores were heritable in twins from divorced and intact families, the heritability estimates in the divorced group were not significantly greater than estimates in the intact group. However, there were differences in nonshared environmental effects, where the magnitude of these environmental influences was larger in the divorced as compared with the intact families. Different dimensions of body dissatisfaction (i.e., negative self-evaluation versus body image perceptions) may interact with environmental risk, such as parental divorce, in discrete ways. Future research should examine this possibility and explore differential gene-environment interactions using diverse measures. © 2015 Wiley Periodicals, Inc.

Parenting Style as a Moderator of the Association between Parenting Behaviors and the Weight Status of Adolescents

ERIC Educational Resources Information Center

Wen, Xu; Hui, Stanley Sai-Chuen

2012-01-01

Based on the contextual model of parenting style, this study aimed to examine whether the associations between parenting behaviors and adolescents' dietary habits, physical activity, and weight status is moderated by parenting style. A total of 1,869 parent-adolescent dyads were recruited in southern China. The adolescents' body mass index,…

Predictors of parental perceptions and concerns about child weight

PubMed Central

Keller, Kathleen L.; Olsen, Annemarie; Kuilema, Laura; Meyermann, Karol; van Belle, Christopher

2012-01-01

Appropriate levels of parental perception and concern about child weight are important components of successful obesity treatment, but the factors that contribute to these attitudes need clarification. The aim of this study was to identify child and parent characteristics that best predict parental perceptions and concerns about child weight. A cross-sectional design was used to assess characteristics of parents (e.g. age, income, and feeding attitudes) and children (e.g. body composition, ad libitum intake, and reported physical activity). Results are reported for 75, 4–6 year-olds from diverse ethnicities. Perceived child weight and concern were measured with the Child Feeding Questionnaire (CFQ). Multiple linear regression was used to identify the best models for perceived child weight and concern. For perceived child weight, the best model included parent age, children’s laboratory intake of sugar-sweetened beverages (SSB) and palatable buffet items, and two measures of child body composition (ratio of trunk fat-to-total fat and ratio of leg fat-to-total fat). For concern, child android/gynoid fat ratio explained the largest amount of variance, followed by restrictive feeding and SSB intake. Parental perceptions and concerns about child weight are best explained by models that account for children’s eating behavior and body fat distribution. PMID:23207190

Global variations in regolith properties on asteroid Vesta from Dawn's low-altitude mapping orbit

NASA Astrophysics Data System (ADS)

Denevi, Brett W.; Beck, Andrew W.; Coman, Ecaterina I.; Thomson, Bradley J.; Ammannito, Eleonora; Blewett, David T.; Sunshine, Jessica M.; de Sanctis, Maria Cristina; Li, Jian-Yang; Marchi, Simone; Mittlefehldt, David W.; Petro, Noah E.; Raymond, Carol A.; Russell, Christopher T.

2016-12-01

We investigate the depth, variability, and history of regolith on asteroid Vesta using data from the Dawn spacecraft. High-resolution (15-20 m pixel-1) Framing Camera images are used to assess the presence of morphologic indicators of a shallow regolith, including the presence of blocks in crater ejecta, spur-and-gully-type features in crater walls, and the retention of small (<300 m) impact craters. Such features reveal that the broad, regional heterogeneities observed on Vesta in terms of albedo and surface composition extend to the physical properties of the upper 1 km of the surface. Regions of thin regolith are found within the Rheasilvia basin and at equatorial latitudes from 0-90°E and 260-360°E. Craters in these areas that appear to excavate material from beneath the regolith have more diogenitic (Rheasilvia, 0-90°E) and cumulate eucrite (260-360°E) compositions. A region of especially thick regolith, where depths generally exceed 1 km, is found from 100-240°E and corresponds to heavily cratered, low-albedo surface with a basaltic eucrite composition enriched in carbonaceous chondrite material. The presence of a thick regolith in this area supports the idea that this is an ancient terrain that has accumulated a larger component of exogenic debris. We find evidence for the gardening of crater ejecta toward more howarditic compositions, consistent with regolith mixing being the dominant form of "weathering" on Vesta.

Pre-bombardment crystallization ages of basaltic clasts from Antarctic howardites EET87503 and EET87513

NASA Technical Reports Server (NTRS)

Nyquist, L. E.; Shih, C.-Y.; Wiesmann, H.; Bansal, B. M.

1994-01-01

Igneous clasts of basaltic eucrites are found in both howardites and polymict eucrites. We have studied the Rb-Sr and Sm-Nd isotopic systematics of a number of such clasts, of metamorphic grades 1-6, using the classification of Takeda and Graham. Here, we report Rb-Sr, (147)Sm-(143)Nd, and (145)Sm-(142)Nd studies of clast, 53 from Antarctic howardite EET87503. Although there is no evidence of disturbance of trace element systematics by Antarctic weathering, the Rb-Sr and conventional Sm-Nd isotopic systematics are severely disturbed, which we ascribe to thermal metamorphism. The Ar-Ar age spectrum shows ages ranging from approximately 3.85-3.55 Ga in an unusual 'down stairstep'. The (146)Sm-(142)Nd systematics, however, show the presence of live (146)Sm(t(sub 1/2) = 103 Ma), with (146)Sm/(144)Sm = 0.0061 +/- 0.0007 at the time of crystallization. This result is very similar to that previously obtained for basaltic clast, 18 from howardite EET87513 (paired with EET87503), which has concordant Rb-Sr and Sm-Nd ages of approximately 4.5 Ga. Thus, the two clasts are nearly the same age, and we conclude further than the EET87503,53 clast crystallized within 33 +/- 19 Ma of the LEW86010 angrite by comparing initial (146)Sm/(144)Sm to that of the angrite. We suggest that disturbances in the isotopic systematics of EET87503,53 are consanguineous with pyroxene homogenization.

Elephant Moraine 87521: The first lunar meteorite composed of predominantly mare material

DOE Office of Scientific and Technical Information (OSTI.GOV)

Warren, P.H.; Kallemeyn, G.W.

1989-12-01

The trace-element chemistry and detailed petrography of brecciated Antarctic meteorite EET87521 reveal that it is not, as originally classified, a eucrite. Its Fe/Mn ratio and bulk Co content are fair higher than expected for a eucrite. Only one known type of extraterrestrial material resembles EET87521 in all important respects for which constraints exist: very-low-Ti (VLT) lunar mare basalts. Even compared to VLT basalts, EET87521 is enriched in REE. However, other varieties of high-alumina, low-Ti mare basalt are known that contain REE at even higher concentrations than EET87521. Several clasts in EET87521 preserve clear vestiges of coarse-grained igneous, possibly orthocumulate, textures.more » Mineralogically, these coarse-grained clasts are diverse; e.g., olivine ranges from Fo{sub 15} in one to Fo{sub 67} in another. One clast with an anomalously fine-grained texture is anorthositic and contains exceptionally Mg-rich pyroxene and Na-poor plagioclase, along with the only FeNi-metal in the thin section. Its FeNi-metals have compositions typical of metals incorporated into lunar soils and polymict breccias as debris from metal-rich meteorites. However, the low Ni and Ir contents of our bulk-rock analysis imply that the proportion of impact-projectile matter in our chip sample is probably small. The moderate degree of lithologic diversity among the lithic lasts and the bulk composition in general indicate that EET87521 is dominated by a single rock type: VLT mare basalt.« less

Predictors of Fat Stereotypes among 9-Year-Old Girls and Their Parents

PubMed Central

Davison, Kirsten Krahnstoever; Birch, Leann Lipps

2008-01-01

Objective To assess familial links in fat stereotypes and predictors of stereotypes among girls and their parents. Research Methods and Procedures Fat stereotypes were assessed using a questionnaire developed for this study. Participants indicated the extent to which they agreed with nine statements about thin people (e.g., thin people are smart) and the same statements about fat people (e.g., fat people are smart). Predictors of fat stereotypes that were examined include weight status (BMI; girls and parents), education (parents), income (parents), self-investment in physical appearance (parents), maladaptive eating attitudes (girls), and parenting practices and peer interactions focused on body shape and weight loss (girls). Results Girls and parents exhibited fat stereotypes. Fathers who were more educated and had a higher family income were more likely to endorse fat stereotypes, as were mothers and fathers with a high investment in their physical appearance. Although no associations were found between girls’ and parents’ fat stereotypes, girls were more likely to endorse fat stereotypes when interactions with parents and peers focused on body shape and weight loss. Girls were also more likely to endorse fat stereotypes when they reported higher levels of maladaptive eating attitudes. No associations were found between weight status and fat stereotypes. Discussion Although there was no association between girls’ and parents’ fat stereotypes, girls were more likely to express negative attitudes about obesity and obese persons when parenting practices and interactions with peers promoted a lean body type, suggesting that there may be an implicit link between the lean ideal and fat stereotypes. PMID:14742846

The effect of low parental warmth and low monitoring on disordered eating in mid-adolescence: Findings from the Australian Temperament Project.

PubMed

Krug, Isabel; King, Ross M; Youssef, George J; Sorabji, Anisha; Wertheim, Eleanor H; Le Grange, Daniel; Hughes, Elizabeth K; Letcher, Primrose; Olsson, Craig A

2016-10-01

To investigate the interactions between low parental warmth and monitoring at age 13-14 years and disordered eating attitudes and behaviours at age 15-16 years. Data on 1300 (667 females) adolescents and their parents were drawn from The Australian Temperament Project (ATP), a 30 year (15 wave) population based longitudinal study of social-emotional development. Parent participants completed surveys on parenting practices in late childhood, and adolescent participants reported disordered eating using the drive for thinness and bulimia subscales of the Eating Disorder Inventory (EDI) and an additional body dissatisfaction scale. Interaction was examined on the additive scale by estimating super-additive risk; i.e., risk in excess of the sum of individual risks. For boys, neither parental warmth or monitoring, nor their interaction, was related to disordered eating. For girls, low parental warmth (alone) was associated with bulimic behaviours. In contrast, exposure to both low monitoring and warmth was associated with ∼3½-fold, ∼4-fold and ∼5-fold increases in the odds of reporting body dissatisfaction, drive for thinness and bulimia, respectively. For body dissatisfaction and drive for thinness, risk associated with joint exposure exceeded the sum of individual risks, suggesting an additive interaction between parenting styles. Further investment in family-level interventions that focus on promoting parental monitoring behaviour and a warm parent-child relationship remain important strategies for preventing a range of disordered eating behaviours in adolescents. Copyright © 2016 Elsevier Ltd. All rights reserved.

Early Intermodal Integration in Offspring of Parents With Psychosis

PubMed Central

Gamma, Franziska; Goldstein, Jill M.; Seidman, Larry J.; Fitzmaurice, Garrett M.; Tsuang, Ming T.; Buka, Stephen L.

2014-01-01

Identifying early developmental indicators of risk for schizophrenia is important for prediction and possibly illness prevention. Disturbed intermodality has been proposed as one important neurodevelopmental risk for schizophrenia. Early intermodal integration (EII) is the infant’s ability to link motility and perception and to relate perception across modalities. We hypothesized that infants of parents with schizophrenia would have more EII abnormalities than infants of healthy parents and that infants of parents with affective psychosis would be intermediate in severity. The New England Family Study high-risk sample, ascertained from community populations, was utilized. Eight-month-old infants of parents with schizophrenia (n = 58), affective psychoses (n = 128), and healthy controls (n = 174) were prospectively assessed. Diagnoses of parents were determined 30 years later blind to offspring data. EII measures were grouped into 3 domains characterizing different aspects of infant development: (1) one’s own body, (2) objects, and (3) social interactions. Results demonstrated that body- and object-related EII abnormalities were significantly increased for infants of parents with schizophrenia compared with control infants and not significantly increased for infants of parents with affective psychoses. EII abnormalities in relation to social interactions were significantly increased in infants of parents with schizophrenia and affective psychoses. Thus, body- and object-related EII abnormalities were most severe in infants of parents with schizophrenia, supporting the importance of intermodality dysfunction as an early indicator of the vulnerability to schizophrenia. Future research should evaluate how this dysfunction evolves with development and its associations with other psychopathological and neurodevelopmental deficits in youth at risk for psychosis. PMID:23986303

Could parental rules play a role in the association between short sleep and obesity in young children?

PubMed

Jones, Caroline H D; Pollard, Tessa M; Summerbell, Carolyn D; Ball, Helen

2014-05-01

Short sleep duration is associated with obesity in young children. This study develops the hypothesis that parental rules play a role in this association. Participants were 3-year-old children and their parents, recruited at nursery schools in socioeconomically deprived and non-deprived areas of a North-East England town. Parents were interviewed to assess their use of sleep, television-viewing and dietary rules, and given diaries to document their child's sleep for 4 days/5 nights. Children were measured for height, weight, waist circumference and triceps and subscapular skinfold thicknesses. One-hundred and eight families participated (84 with complete sleep data and 96 with complete body composition data). Parental rules were significantly associated together, were associated with longer night-time sleep and were more prevalent in the non-deprived-area compared with the deprived-area group. Television-viewing and dietary rules were associated with leaner body composition. Parental rules may in part confound the association between night-time sleep duration and obesity in young children, as rules cluster together across behavioural domains and are associated with both sleep duration and body composition. This hypothesis should be tested rigorously in large representative samples.

Perceptions of Body Image by Persons with Prader-Willi Syndrome and Their Parents

ERIC Educational Resources Information Center

Napolitano, Deborah A.; Zarcone, Jennifer; Nielsen, Sarah; Wang, Hongyue; Caliendo, Jillian Maynard

2010-01-01

Prader-Willi syndrome is a genetic disorder characterized by obesity. The Figure Rating Scale (Stunkard, Sorensen, & Schulsinger, 1983) was completed by 43 individuals with this syndrome to determine their level of dissatisfaction with their body. Their parents also completed this scale regarding their child to determine whether they were…

Is All Classroom Conduct Equal?: Teacher Contact with Parents of Racial/Ethnic Minority and Immigrant Adolescents

ERIC Educational Resources Information Center

Cherng, Hua-Yu Sebastian

2016-01-01

Background/Context: Parental involvement is a key ingredient in the educational success of students and an integral component of involvement is teacher-parent communication. One body of research finds that minority immigrant parents face barriers in interacting with schools, and communicate less with schools than native-born White parents.…

The Effects of Social Norms on Parents' Reading Behaviour at Home with Their Child

ERIC Educational Resources Information Center

Colgate, Orla; Ginns, Paul

2016-01-01

Currently, parental involvement research considers parents as individuals, and gives little consideration to them as a collective body, including how, as a group, they might influence each other. This study examined the influence of parent social norms on parents' home reading behaviour with their child. Two quasi-experiments conducted in two…

Late metal-silicate separation on the IAB parent asteroid: Constraints from combined W and Pt isotopes and thermal modelling

NASA Astrophysics Data System (ADS)

Hunt, Alison C.; Cook, David L.; Lichtenberg, Tim; Reger, Philip M.; Ek, Mattias; Golabek, Gregor J.; Schönbächler, Maria

2018-01-01

The short-lived 182Hf-182W decay system is a powerful chronometer for constraining the timing of metal-silicate separation and core formation in planetesimals and planets. Neutron capture effects on W isotopes, however, significantly hamper the application of this tool. In order to correct for neutron capture effects, Pt isotopes have emerged as a reliable in-situ neutron dosimeter. This study applies this method to IAB iron meteorites, in order to constrain the timing of metal segregation on the IAB parent body. The ε182W values obtained for the IAB iron meteorites range from -3.61 ± 0.10 to -2.73 ± 0.09. Correlating εiPt with ε182W data yields a pre-neutron capture ε182W of -2.90 ± 0.06. This corresponds to a metal-silicate separation age of 6.0 ± 0.8 Ma after CAI for the IAB parent body, and is interpreted to represent a body-wide melting event. Later, between 10 and 14 Ma after CAI, an impact led to a catastrophic break-up and subsequent reassembly of the parent body. Thermal models of the interior evolution that are consistent with these estimates suggest that the IAB parent body underwent metal-silicate separation as a result of internal heating by short-lived radionuclides and accreted at around 1.4 ± 0.1 Ma after CAIs with a radius of greater than 60 km.

Search for a Differentiated Asteroid Family

NASA Astrophysics Data System (ADS)

Thomas, Cristina A.; Lim, Lucy F.; Trilling, David E.; Moskovitz, Nicholas

2014-08-01

Dynamical asteroid families resulting from catastrophic disruptions represent the interiors of their former parent bodies. Differentiation of a large initially chondritic parent body is expected to produce an ``onion shell" object with a metal core, a thick olivine-rich mantle, and a thin basaltic crust. However, instead of the mineralogical diversity expected from the disruption of a differentiated parent body, most asteroid families tend to show similar spectra among the members. Moreover, spectra of metal-like materials and olivine-dominated assemblages have not been detected in asteroid families in the Main Belt and the expected mantle material is missing from the meteorite record. The deficit of olivine-rich mantle material in the meteorite record and in asteroid observations is known as the ``Missing Mantle" problem. For years the best explanation for the lack of mantle material has been the ``battered to bits" hypothesis that states that all differentiated parent bodies (aside from Vesta) were disrupted very early in the solar system and the resulting olivine-rich material was collisionally broken down until the object diameters fell below our observational limits. However, in a new, competing, hypothesis, Elkins-Tanton et al. (2013) has suggested that previous work has overestimated the amount of olivine produced by the differentiation of a chondritic parent body. We propose to obtain visible spectra of asteroids within the Massalia, Merxia, and Agnia S-type families to search for compositional variations that are indicators of differentiation and to quantitatively constrain the two competing ``Missing Mantle" hypotheses.

Parenting styles, feeding styles, and their influence on child obesogenic behaviors and body weight. A review.

PubMed

Vollmer, Rachel L; Mobley, Amy R

2013-12-01

With recommendations to include parents as targets for childhood obesity interventions, there is a need to review the relationship of general parenting influences on childhood obesity. Therefore, the aim of this review is to examine the existing literature regarding the influence of parenting style and/or feeding styles on childhood obesogenic behaviors and body weight. Research articles related to parenting style (n=40) and parental feeding style (n=11) were identified and reviewed. An authoritative style appears to be the most protective parenting and feeding style while the indulgent feeding style is consistently associated with negative health outcomes. Overall, results for parenting style studies are inconsistent due to differences in conceptualization and measurement, while the results for feeding styles are much more cohesive. The literature is lacking in the ability to describe the interplay between parenting and feeding styles and child obesity risk. Recommendations for future research and interventions are discussed in regards to feeding style and influences on childhood obesity. Copyright © 2013 Elsevier Ltd. All rights reserved.

Sex-Differences in the Metabolic Health of Offspring of Parents with Diabetes: A Record-Linkage Study

PubMed Central

Aldhous, Marian C.; Reynolds, Rebecca M.; Campbell, Archie; Linksted, Pamela; Lindsay, Robert S.; Smith, Blair H.; Seckl, Jonathan R.; Porteous, David J.; Norman, Jane E.

2015-01-01

Maternal diabetes in pregnancy affects offspring health. The impact of parental diabetes on offspring health is unclear. We investigated the impact of parental diabetes on the metabolic-health of adult-offspring who did not themselves have diabetes. Data from the Generation Scotland: Scottish Family Health Study, a population-based family cohort, were record-linked to subjects’ own diabetes medical records. From F0-parents, we identified F1-offspring of: mothers with diabetes (OMD, n = 409), fathers with diabetes (OFD, n = 468), no parent with diabetes (ONoPD, n = 2489). Metabolic syndrome, body, biochemical measurements and blood-pressures were compared between F1-offspring groups by sex. A higher proportion of female OMD had metabolic syndrome than female OFD or ONoPD (P<0.0001). In female offspring, predictors of metabolic syndrome were: having a mother with diabetes (OR = 1.78, CI 1.03–3.07, [reference ONoPD]), body mass index (BMI, OR = 1.21, CI 1.13–1.30) and age (OR = 1.03, CI 1.01–1.06). In male offspring, predictors of metabolic syndrome were: BMI (OR = 1.18, CI 1.09–1.29) and percent body-fat (OR = 1.12, CI 1.05–1.19). In both sexes, OMD had higher blood-pressures than OFD (P<0.0001). In females, OMD had higher glucose (P<0.0001) and percent body-fat (P<0.0001) compared with OFD or ONoPD. OMD and OFD both had increased waist-measurements (P<0.0001), BMI (P<0.0001) and percent body-fat (P<0.0001) compared with ONoPD. Female OMD and OFD had lower HDL-cholesterol levels (P<0.0001) than female ONoPD. Parental diabetes is associated with higher offspring-BMI and body-fat. In female offspring, maternal diabetes increased the odds of metabolic syndrome, even after adjusting for BMI. Further investigations are required to determine the mechanisms involved. PMID:26308734

Parental education associations with children's body composition: mediation effects of energy balance-related behaviors within the ENERGY-project.

PubMed

Fernández-Alvira, Juan M; te Velde, Saskia J; De Bourdeaudhuij, Ilse; Bere, Elling; Manios, Yannis; Kovacs, Eva; Jan, Natasa; Brug, Johannes; Moreno, Luis A

2013-06-21

It is well known that the prevalence of overweight and obesity is considerably higher among youth from lower socio-economic families, but there is little information about the role of some energy balance-related behaviors in the association between socio-economic status and childhood overweight and obesity. The objective of this paper was to assess the possible mediation role of energy balance-related behaviors in the association between parental education and children's body composition. Data were obtained from the cross sectional study of the "EuropeaN Energy balance Research to prevent excessive weight Gain among Youth" (ENERGY) project. 2121 boys and 2516 girls aged 10 to 12 from Belgium, Greece, Hungary, the Netherlands, Norway, Slovenia and Spain were included in the analyses. Data were obtained via questionnaires assessing obesity related dietary, physical activity and sedentary behaviors and basic anthropometric objectively measured indicators (weight, height, waist circumference). The possible mediating effect of sugared drinks intake, breakfast consumption, active transportation to school, sports participation, TV viewing, computer use and sleep duration in the association between parental education and children's body composition was explored via MacKinnon's product-of-coefficients test in single and multiple mediation models. Two different body composition indicators were included in the models, namely Body Mass Index and waist circumference. The association between parental education and children's body composition was partially mediated by breakfast consumption, sports participation, TV viewing and computer use. Additionally, a suppression effect was found for sugared drinks intake. No mediation effect was found for active transportation and sleep duration. The significant mediators explained a higher proportion of the association between parental education and waist circumference compared to the association between parental education and BMI. Tailored overweight and obesity prevention strategies in low SES preadolescent populations should incorporate specific messages focusing on the importance of encouraging daily breakfast consumption, increasing sports participation and decreasing TV viewing and computer use. However, longitudinal research to support these findings is needed.

Magnetic Evidence for a Partially Differentiated Carbonaceous Chondrite Parent Body and Possible Implications for Asteroid 21 Lutetia

NASA Astrophysics Data System (ADS)

Weiss, Benjamin; Carporzen, L.; Elkins-Tanton, L.; Shuster, D. L.; Ebel, D. S.; Gattacceca, J.; Binzel, R. P.

2010-10-01

The origin of remanent magnetization in the CV carbonaceous chondrite Allende has been a longstanding mystery. The possibility of a core dynamo like that known for achondrite parent bodies has been discounted because chondrite parent bodies are assumed to be undifferentiated. Here we report that Allende's magnetization was acquired over several million years (Ma) during metasomatism on the parent planetesimal in a > 20 microtesla field 8-9 Ma after solar system formation. This field was present too recently and directionally stable for too long to have been the generated by the protoplanetary disk or young Sun. The field intensity is in the range expected for planetesimal core dynamos (Weiss et al. 2010), suggesting that CV chondrites are derived from the outer, unmelted layer of a partially differentiated body with a convecting metallic core (Elkins-Tanton et al. 2010). This suggests that asteroids with differentiated interiors could be present today but masked under chondritic surfaces. In fact, CV chondrites are spectrally similar to many members of the Eos asteroid family whose spectral diversity has been interpreted as evidence for a partially differentiated parent asteroid (Mothe-Diniz et al. 2008). CV chondrite spectral and polarimetric data also resemble those of asteroid 21 Lutetia (e.g., Belskaya et al. 2010), recently encountered by the Rosetta spacecraft. Ground-based measurements of Lutetia indicate a high density of 2.4-5.1 g cm-3 (Drummond et al. 2010), while radar data seem to rule out a metallic surface composition (Shepard et al. 2008). If Rosetta spacecraft measurements confirm a high density and a CV-like surface composition for Lutetia, then we propose Lutetia may be an example of a partially differentiated carbonaceous chondrite parent body. Regardless, the very existence of primitive achondrites, which contain evidence of both relict chondrules and partial melting, are prima facie evidence for the formation of partially differentiated bodies.

Parent body depth-pressure-temperature relationships and the style of the ureilite anatexis

NASA Astrophysics Data System (ADS)

Warren, Paul H.

2012-02-01

New analyses of mafic silicates from 14 ureilite meteorites further constrain a strong correlation (Singletary and Grove 2003) between olivine-core Fo ratio and the temperature of equilibration (TE) recorded by the composition of pigeonite. This correlation may be compared with relationships implied by various postulated combinations of Fo and pressure P in models for ureilite genesis by a putative process of anatectic (depth-linked, P-controlled) smelting. In such models, any combination of Fo and P together fixes the temperature of smelting. Agreement between the observed correlation and these models is poor. The anatectic smelting model also carries implausible implications for the depth range at which ureilites of a given composition (Fo) form. Actual ureilites (and polymict ureilite clasts: Downes et al. 2008) show a distribution strongly skewed toward the low-Fo end of the compositional range, with approximately 58% in the range Fo76-81. In contrast, the P-controlled smelting model implies that the Fo76-81 region is a small fraction of the volume of the parent body: not more than 3.2%, in a model consistent with the Fo-TE observations; and even ignoring the Fo-TE evidence not more than 11% (percentages cited require optimal assumptions concerning the size of the parent body). This region also must occur deep within the body, where no straightforward model would imply a strong bias in the impact-driven sampling process. The ureilites did not derive preponderantly from one atypical “largest offspring” disruption survivor, because cooling history evidence shows that after the disruption (whose efficiency was increased by gas jetting), all of the known ureilites cooled in bodies that were tiny (mass of order 10-9) in comparison with the precursor body. The Ca/Al ratio of the ureilite starting matter cannot be 2.5 times chondritic, as has been suggested, unless the part of the body from which ureilites come is at most 50% of the whole body. Published variants of the anatectic, P-controlled smelting model have the ureilites coming from a region that is >50 vol% of their parent body; and to invoke a larger body would have the drawback of implying that the Fo76-81 spike represents an even smaller fraction of the parent body's interior. The ureilites' moderate depletions in incompatible elements are difficult to reconcile with a fractional fusion model. It is not plausible that melt formed grossly out of equilibrium with the medium-sized ureilite crystals. The alternative to pressure-controlled smelting, i.e., a model of gasless or near-gasless anatexis, has very different implications for the size and evolution of the original parent body. To yield internal pressures prohibitive of smelting in even the shallowest and most ferroan portion of its anatectic mantle, the body would have to be larger than roughly 690 km in diameter. A 400 km body would have approximately 12 vol% of the interior (or 13 vol% of the interior apart from the thermal “skin” that never undergoes anatexis) prone, if both extremely shallow and extremely ferroan, to mild smelting. Gasless anatexis also implies that this large parent body was compositionally, at least in terms of mg, grossly heterogeneous before anatexis, probably (in view of the oxygen isotopic diversity) as a result of mixed accretion.

Disentangling the associations between parental BMI and offspring body composition using the four‐component model

PubMed Central

Grijalva‐Eternod, Carlos; Cortina‐Borja, Mario; Williams, Jane; Fewtrell, Mary; Wells, Jonathan

2016-01-01

ABSTRACT Objectives This study sets out to investigate the intergenerational associations between the body mass index (BMI) of parents and the body composition of their offspring. Methods The cross‐sectional data were analyzed for 511 parent–offspring trios from London and south‐east England. The offspring were aged 5–21 years. Parental BMI was obtained by recall and offspring fat mass and lean mass were obtained using the four‐component model. Multivariable regression analysis, with multiple imputation for missing paternal values was used. Sensitivity analyses for levels of non‐paternity were conducted. Results A positive association was seen between parental BMI and offspring BMI, fat mass index (FMI), and lean mass index (LMI). The mother's BMI was positively associated with the BMI, FMI, and LMI z‐scores of both daughters and sons and of a similar magnitude for both sexes. The father's BMI showed similar associations to the mother's BMI, with his son's BMI, FMI, and LMI z‐scores, but no association with his daughter. Sensitivity tests for non‐paternity showed that maternal coefficients remained greater than paternal coefficients throughout but there was no statistical difference at greater levels of non‐paternity. Conclusions We found variable associations between parental BMI and offspring body composition. Associations were generally stronger for maternal than paternal BMI, and paternal associations appeared to differ between sons and daughters. In this cohort, the mother's BMI was statistically significantly associated with her child's body composition but the father's BMI was only associated with the body composition of his sons. Am. J. Hum. Biol. 28:524–533, 2016. © 2016 The Authors American Journal of Human Biology Published by Wiley Periodicals, Inc. PMID:26848813

Observed parent-child feeding dynamics in relation to child body mass index and adiposity.

PubMed

Johnson, C M; Henderson, M S; Tripicchio, G; Rozin, P; Heo, M; Pietrobelli, A; Berkowitz, R I; Keller, K L; Faith, M S

2018-04-01

Restrictive feeding is associated with child overweight; however, the majority of studies used parent-report questionnaires. The relationship between child adiposity measures and directly observed parent and child behaviours were tested using a novel behavioural coding system (BCS). Data from 109 children, participants in a twin study and their mothers, were analyzed. Parent-child dyads were video-recorded twice in the laboratory, while children ate ad libitum from a buffet lunch. Mother and child behaviours were assessed using the BCS. Height, body weight and body fat were directly measured for each child. Associations between child adiposity measures and average BCS behaviour (i.e. pooled across visits) were tested using partial correlations adjusting for child age. Regarding discouragement prompts, child body mass index (BMI) z-score was significantly associated with a greater rate of total discouragements (per minute, min -1 ), nonverbal discouragements (min -1 ) and temporary (delay) discouragements (min -1 ) (p < 0.05). Child percent body fat was associated with greater nonverbal discouragements (min -1 ). Regarding encouragement prompts, child BMI z-score was significantly associated with a greater rate of total encouragements (min -1 ), nonverbal encouragements (min -1 ) and reward encouragements (min -1 ). Child BMI z-score and percent body fat were both positively associated with greater maternal health encouragements (min -1 ). Associations with encouragement to eat prompts were no longer significant when accounting for the dependence among twins (being part of the same family). Heavier children received greater maternal discouragements to eat and, with qualifications, encouragements to eat. The role of nonverbal parenting cues warrants further research regarding child eating regulation and obesity. © 2017 World Obesity Federation.

Iron meteorites as remnants of planetesimals formed in the terrestrial planet region.

PubMed

Bottke, William F; Nesvorný, David; Grimm, Robert E; Morbidelli, Alessandro; O'Brien, David P

2006-02-16

Iron meteorites are core fragments from differentiated and subsequently disrupted planetesimals. The parent bodies are usually assumed to have formed in the main asteroid belt, which is the source of most meteorites. Observational evidence, however, does not indicate that differentiated bodies or their fragments were ever common there. This view is also difficult to reconcile with the fact that the parent bodies of iron meteorites were as small as 20 km in diameter and that they formed 1-2 Myr earlier than the parent bodies of the ordinary chondrites. Here we show that the iron-meteorite parent bodies most probably formed in the terrestrial planet region. Fast accretion times there allowed small planetesimals to melt early in Solar System history by the decay of short-lived radionuclides (such as 26Al, 60Fe). The protoplanets emerging from this population not only induced collisional evolution among the remaining planetesimals but also scattered some of the survivors into the main belt, where they stayed for billions of years before escaping via a combination of collisions, Yarkovsky thermal forces, and resonances. We predict that some asteroids are main-belt interlopers (such as (4) Vesta). A select few may even be remnants of the long-lost precursor material that formed the Earth.

A large planetary body inferred from diamond inclusions in a ureilite meteorite.

PubMed

Nabiei, Farhang; Badro, James; Dennenwaldt, Teresa; Oveisi, Emad; Cantoni, Marco; Hébert, Cécile; El Goresy, Ahmed; Barrat, Jean-Alix; Gillet, Philippe

2018-04-17

Planetary formation models show that terrestrial planets are formed by the accretion of tens of Moon- to Mars-sized planetary embryos through energetic giant impacts. However, relics of these large proto-planets are yet to be found. Ureilites are one of the main families of achondritic meteorites and their parent body is believed to have been catastrophically disrupted by an impact during the first 10 million years of the solar system. Here we studied a section of the Almahata Sitta ureilite using transmission electron microscopy, where large diamonds were formed at high pressure inside the parent body. We discovered chromite, phosphate, and (Fe,Ni)-sulfide inclusions embedded in diamond. The composition and morphology of the inclusions can only be explained if the formation pressure was higher than 20 GPa. Such pressures suggest that the ureilite parent body was a Mercury- to Mars-sized planetary embryo.

Collisional fragmentation of asteroids and its implication on the physical properties of Near-Earth Objects

NASA Astrophysics Data System (ADS)

Michel, P.

Collisions are at the origin of catastrophic disruptions in the asteroid Main Belt. This is witnessed by the observation of asteroid families, each composed of asteroids which originated from a single parent body, broken-up by a collision with another asteroid. Understanding the collisional process and its outcome properties is not only necessary in order to study the collisional evolution of small body population or the planetary formation, it is also strongly required in the context of mitigation strategies aimed at deviating a threatening asteroid. In the last three years, for the first time we have successfully performed numerical simulations of high speed collisions between small bodies which account for the production of gravitationally reaccumulated bodies. More precisely, we have developped a procedure which divides the process into two phases. Using a 3D SPH hydrocode, the fragmentation of the solid target through crack propagation is first computed. Then the simulation of the gravitational evolution and possible piecewise reaccumulation of the parent body is performed using the parallel N-body code pkdgrav. Our first simulations using monolithic parent bodies have succeeded in reproducing fundamental properties of some well-identified asteroid families, showing that gravitational re-accumulations following disruptive collisions are the key process accounting for the existence of asteroid families. Then, we have investigated the effect of the internal structure of the parent body on the outcome properties. We have thus shown that family parent bodies are likely to have already been pre-shattered by small impacts before being disrupted by a major event. We then suggested that the most likely internal structure of large asteroids in the main belt is not monolithic but rather composed of macroscopic fractures and voids. We will make a review of these simulations in three different impact regimes, from highly catastrophic to barely disruptive. In particular we will show the sensitivity of the resulting family characteristics upon the internal structure of the parent body. According to our current understanding, most NEOs are certainly fragments of larger asteroids of the Main Belt, injected either directly or by diffusion into main resonances that transported them to Earth-crossing orbits. According to our simulations, most NEOs with diameter larger than several hundreds of meters should then correspond to gravitational aggregates. Given the crucial role of the internal structure on the impact outcome, this has important implications in the development of efficient mitigation strategies.

The effectiveness of lifestyle triple P in the Netherlands: a randomized controlled trial.

PubMed

Gerards, Sanne M P L; Dagnelie, Pieter C; Gubbels, Jessica S; van Buuren, Stef; Hamers, Femke J M; Jansen, Maria W J; van der Goot, Odilia H M; de Vries, Nanne K; Sanders, Matthew R; Kremers, Stef P J

2015-01-01

Lifestyle Triple P is a general parenting intervention which focuses on preventing further excessive weight gain in overweight and obese children. The objective of the current study was to assess the effectiveness of the Lifestyle Triple P intervention in the Netherlands. We used a parallel randomized controlled design to test the effectiveness of the intervention. In total, 86 child-parent triads (children 4-8 years old, overweight or obese) were recruited and randomly assigned (allocation ratio 1:1) to the Lifestyle Triple P intervention or the control condition. Parents in the intervention condition received a 14-week intervention consisting of ten 90-minute group sessions and four individual telephone sessions. Primary outcome measure was the children's body composition (BMI z-scores, waist circumference and skinfolds). The research assistant who performed the measurements was blinded for group assignment. Secondary outcome measures were the children's dietary behavior and physical activity level, parenting practices, parental feeding style, parenting style, and parental self-efficacy. Outcome measures were assessed at baseline and 4 months (short-term) and 12 months (long-term) after baseline. Multilevel multiple regression analyses were conducted to determine the effect of the intervention on primary and secondary outcome measures. No intervention effects were found on children's body composition. Analyses of secondary outcomes showed positive short-term intervention effects on children's soft-drink consumption and parental responsibility regarding physical activity, encouragement to eat, psychological control, and efficacy and satisfaction with parenting. Longer-term intervention effects were found on parent's report of children's time spent on sedentary behavior and playing outside, parental monitoring food intake, and responsibility regarding nutrition. Although the Lifestyle Triple P intervention showed positive effects on some parent reported child behaviors and parenting measures, no effects were visible on children's body composition or objectively measured physical activity. Several adjustments of the intervention content are recommended, for example including a booster session. Nederlands Trial Register NTR 2555.

Expectations of Parents of First-Year Students regarding Collegiate Teaching and Caring at a Public University

ERIC Educational Resources Information Center

Spearman, Christina J.

2010-01-01

Parental involvement in higher education has greatly increased, specifically in the last 30 years. Some parents are hyper-involved in their children's lives, and educational leaders often spend almost as much time working with parents as they do students. The body of literature on parental involvement in higher education is limited. Therefore, the…

Parents of Elementary School Students Weigh in on Height, Weight, and Body Mass Index Screening at School

ERIC Educational Resources Information Center

Kubik, Martha Y.; Fulkerson, Jayne A.; Story, Mary; Rieland, Gayle

2006-01-01

School-based body mass index (BMI) screening and parent notification programs have been recommended as a childhood overweight prevention strategy. However, there are little empirical data available to guide decision making about the acceptability and safety of programs. A pilot study was conducted using a quasiexperimental research design. In fall…

On possible parent bodies of Innisfree, Lost City and Prgibram meteorites.

NASA Astrophysics Data System (ADS)

Rozaev, A. E.

1994-12-01

Minor planets 1981 ET3 and Seleucus are possible parent bodies of Innisfree and Lost City meteorites, asteroid Mithra is the most probable source of Prgibram meteorite. The conclusions are based on the Southworth - Hawkins criterion with taking into account of the motion constants (Tisserand coefficient, etc.) and minimal distances between orbits at present time.

Parental Acceptance and Rejection: Theory, Measures, and Research in the Arab World

ERIC Educational Resources Information Center

Ahmed, Ramadan A.; Rohner, Ronald P.; Khaleque, Abdul; Gielen, Uwe P.

2010-01-01

Purpose. The purpose of this article is to summarize the rich and growing body of research that draws from parental acceptance-rejection theory (PARTheory) and associated measures as used throughout the Arab world. Methodology. This body of work includes more than 100 studies that explore the reliability and validity of Arabic adaptations of…

Meteorites and their parent bodies: Evidence from oxygen isotopes

NASA Technical Reports Server (NTRS)

Clayton, R. N.

1978-01-01

Isotopic abundance variations among meteorites are used to establish genetic associations between meteorite classes. Oxygen isotope distributions between group II E irons with H-group ordinary chondrites and enstatic meteorites indicate that the parent bodies were formed out of pre-solar material that was not fully mixed at the time condensation occurred within the solar nebula.

Parental Bonds, Anxious Attachment, Media Internalization, and Body Image Dissatisfaction: Exploring a Mediation Model

ERIC Educational Resources Information Center

Cheng, Hsiu-Lan; Mallinckrodt, Brent

2009-01-01

The first purpose of this study was to investigate direct links between body image dissatisfaction (BID) in college women and their memories of either parent as cold and emotionally aloof. Theory, clinical case evidence, and a small (but growing) number of studies support these links. After estimating the strength of the associations between…

Meteoritic parent bodies - Nature, number, size and relation to present-day asteroids

NASA Technical Reports Server (NTRS)

Lipschutz, Michael E.; Gaffey, Michael J.; Pellas, Paul

1989-01-01

The relationship between meteoritic parent bodies and the present-day asteroids is discussed. Results on oxygen isotopic signatures and chemical distinctions among meteorite classes indicate that meteorites derive from a small number of parent bodies relative to the number of asteroids. The spectral properties of the ordinary chondrites and similar inclusions in meteoritic breccias differ from those of the abundant S asteroids (with no process known that can account for these differences); the closest spectral analogs of these chondrites are the rare near-earth Q-type asteroids. These facts lead to the question of why abundant meteorites have rare asteroidal analogs, while the abundant asteroids have rare meteoritic analogs. This question constitutes a prime topic for future studies.

Characteristics and formation of amino acids and hydroxy acids of the Murchison meteorite

NASA Technical Reports Server (NTRS)

Cronin, J. R.; Cooper, G. W.; Pizzarello, S.

1995-01-01

Eight characteristics of the unique suite of amino acids and hydroxy acids found in the Murchison meteorite can be recognized on the basis of detailed molecular and isotopic analyses. The marked structural correspondence between the alpha-amino acids and alpha-hydroxy acids and the high deuterium/hydrogen ratio argue persuasively for their formation by aqueous phase Strecker reactions in the meteorite parent body from presolar, i.e., interstellar, aldehydes, ketones, ammonia, and hydrogen cyanide. The characteristics of the meteoritic suite of amino acids and hydroxy acids are briefly enumerated and discussed with regard to their consonance with this interstellar-parent body formation hypothesis. The hypothesis has interesting implications for the organic composition of both the primitive parent body and the presolar nebula.

Phosphate-Silicate Inclusions in Chaunskij: How Diverse are They?

NASA Astrophysics Data System (ADS)

Petaev, M. I.; Clarke, R. S., Jr.; Jarosewich, E.; Lipschutz, M. E.; Wang, M.-S.; Davis, A. M.; Steele, I. M.; Olsen, E. J.; Wood, J. A.

1993-07-01

The Chaunskij meteorite was found in 1985 and was recently classified as the most highly metamorphosed, shock-modified, and metal-rich mesosiderite [1]. It contains ~10 vol% mono- and polymineralic troilite-phosphate-silicate inclusions, micrometers to centimeters in size. Metal in Chaunskij displays a mesosiderite structure and is described in some detail in an accompanying paper [2]. Here we present new data on polymineralic inclusions that shed additional light on their origin. Two dominant silicate lithologies have been found in the inclusions. One, making up the largest inclusion (2.2 x 1.7 cm), consists of a fine-grained (20-30 micrometers) aggregate of anhedral pyroxene, subhedral plagioclase laths, and silica, with larger poikilitic grains of the first two minerals. Whitlockite is minor. Textures vary from microophitic to xenoblastic. This lithology, called "igneous," also contains rare primary clasts enriched in pyroxene, whose boundaries are almost unresolvable from the ground mass in transmitted light. The second, "metamorphic" lithology occurs as separate small inclusions and as larger areas in intimate contact with the "igneous" lithology in the largest inclusion. This lithology is a fine-grained (typically 30-50 micrometers) xenoblastic intergrowth of low-Ca pyroxene, whitlockite, and cordierite, with rare larger porphyritic grains of the first two minerals. Porphyritic pyroxene grain edges are generally irregular, indicative of reaction with the ground mass. Plagioclase is present only as a rare accessory mineral. Minor minerals in both lithologies are silica, kamacite, taenite, troilite, chromite, ilmenite, and rutile. Rare grains of pyrophanite, zircon, alabandite, stanfieldite, and a graftonite-farringtonite mineral are also present in the inclusions. Mineral compositions of small inclusions are more diverse than those characteristic of the "igneous" and "metamorphic" lithologies. Many of them consist of cordierite, pyroxene, and whitlockite intergrowths, with or without silica and opaque minerals. However, some inclusions do not match the mineralogies of "igneous" or "metamorphic" lithologies. They consist of cordierite only (inclusion #1-10); cordierite and silica (#1-18); silica, whitlockite, and troilite with minor Al-rich chromite and rare pyroxene (#4- 5A); plagioclase and whitlockite (#4-5D); and silica and whitlockite (#4-6E). Mineral compositions vary considerably both between and within all inclusions. No systematic differences between separate inclusions were found. Compositions of pyroxene and plagioclase match those of mesosideritic minerals. The chromite and ilmenite display systematic variations in MgO, MnO, Al(sub)2O(sub)3 and V(sub)2O(sub)3 contents, suggestive of a precursor material consisting of a series of basaltic rocks. The bulk chemical composition of the largest silicate inclusion, recalculated to the silicate fraction only, is very close to that of eucrites and mesosiderites except for a large enrichment in P and volatile chalcophiles. Major-element and REE chemistry and bulk mineralogy point to cumulate eucrites as the precursor of the silicate inclusions. This precursor was apparently slightly fractionated during the remelting event inferred by the structure of the "igneous" lithology. The "metamorphic" lithology apparently was formed due to reaction between silicates and phosphorus dissolved in the metal: Px + An + P + O --> Cord + Q + Whit. This reaction took place under ~700 degrees C and ~4 kbar [3] in the interior of the Chaunskij parent body. Compositions and textures of small inclusions suggest that the metamorphic reaction took place before the incorporation of the inclusions into the piece of metal making up the Chaunskij main mass. References: [1] Petaev M. I. et al. (1993) LPS XXIV, 1131-1132. [2] Clarke R. S. Jr. et al., this volume. [3] Petaev M. I. et al. (1992) Meteoritics, 27, 276-277.

Antarctic Meteorite Newsletter. Volume 22

NASA Technical Reports Server (NTRS)

Satterwhite, Cecilia (Editor); Lindstrom, Marilyn (Editor)

1999-01-01

This Newsletter Contains Classifications of 143 New Meteorites from the 1997 ANSMET Collection. Descriptions are given for 6 meteorites;2 eucrites, and 4 ordinary chondrites. We don't expect much excitement from the rest of the 1997 collection. JSC has examined another 100 meteorites to send to the Smithsonian for classification and they appear to be more of the same LL5 shower. However, past experience tells us that there will be some treasures hidden in the remaining samples. Hope rings eternal, but we can't wait to see the 1998 collection described below.

The distribution of zirconium and hafnium in terrestrial rocks, meteorites and the moon

NASA Technical Reports Server (NTRS)

Ehmann, W. D.; Chyi, L. L.; Garg, A. N.; Ali, M. Z.

1979-01-01

It is shown that Zr and Hf are not always fractionated in terrestrial igneous differentiation or regional metamorphism. Data do support a Zr-Hf fractionation in the differentiation of the alkali olivine magma at St. Helena Island. A strong Zr-Hf fractionation exists among lunar rocks and minerals. Ilmenite is an excellent concentrator of Zr and Hf and always exhibits high Zr/Hf ratios. Chondritic meteorites exhibit rather uniform Zr abundances and Zr/Hf ratios but a distinct Zr-Hf fractionation is observed among the eucrite and diogenite achondrites.

The Erevan howardite: Petrology of glassy clasts and mineral chemistry

NASA Technical Reports Server (NTRS)

Nazarov, M. A.; Ariskin, A. A.

1993-01-01

The Erevan howardite is a polymict regolith breccia containing xenoliths of carbonaceous chondrites. In this work, we studied glassy clasts, which could be considered as primary quenched melts, and mineral chemistry of the breccia. The study reveals that the Erevan howardite consists of common rocks of the HED suite. However, unique glassy clasts, which are present in some eucritic melts, were identified. The mineral chemistry and the simulation of crystallization of the melts suggest that the compositions of the melts reflect those of some primary lithologies of EPB.

Children with food refusal: an assessment of parental eating attitudes and their styles of coping with stress.

PubMed

Tan, Seda; Yilmaz, Ayse Esra; Karabel, Musemma; Kara, Semra; Aldemir, Seçil; Karabel, Duran

2012-05-01

In this study, we aimed to assess the eating attitudes and stress coping styles of parents whose children presented to the clinic complaining of food refusal. The parents of 31 children aged ≥3 years, presented to the clinic with the complaint of food refusal. The control group consisted of 30 healthy children with no prior history of food refusal, and their parents. In both groups, birth features, body mass indexes (BMIs), eating attitudes and stress coping styles of the parents were assessed. The parents of both groups were studied, in part utilizing the eating attitudes test (EAT), and the coping styles of stress scale (CSSS). Our study found that body weights and BMI values of the fathers in the study group were significantly lower than fathers in the control group. There was no significant difference in EAT scores between the two groups; however, where the children's body weight and height for age percentile was under 25%, the parents had significantly lower EAT scores. When CSSS scores were assessed, the optimistic approach score of the mother and the self-confident score of the father were found to be significantly high in both groups. The parental perception and definition of eating problems does not necessarily indicate the presence of an eating disorder in a child. In fact, the eating attitudes of the fathers were related to the low percentile weight and height values of the children, and a child's food refusal was not dependent on the stress coping style used by the parent. Copyright © 2012. Published by Elsevier B.V.

Paleomagnetic Evidence for Partial Differentiation of the Silicate-Bearing IIE Iron Meteorite Parent Body

NASA Astrophysics Data System (ADS)

Maurel, C.; Bryson, J. F. J.; Weiss, B. P.; Scholl, A.

2016-12-01

The identification of dozens of petrologically diverse chondritic and achondritic meteoritic groups indicates that a diversity of planetesimals formed in the early solar system. It is commonly thought that planetesimals formed as either unmelted or else fully differentiated bodies, implying that chondrites and achondrites cannot have originated on a single body. However, it has been suggested that partially melted bodies with chondritic crusts and achondritic interiors may also have formed. This alternative proposal is supported by the recent identification of post-accretional remanent magnetization in CV, H chondrites, and also possibly in CM chondrites, which has been interpreted as possible evidence for a core dynamo on their parent bodies. Other piece of evidence suggesting the existence of partially differentiated bodies is the existence of the silicate-bearing IIE iron meteorites. The IIEs are composed of a Fe-Ni alloy matrix containing a mixture of chondritic, primitive achondritic, and chondritic silicate inclusions that likely formed on a single parent body. Therefore, IIEs may sample all three putative layers of a layered, partially differentiated body. On the other hand, the siderophile element compositions of the matrix metal demonstrate that it is not the product of fractional crystallization of a molten core. This suggests that the matrix metal is derived from isolated reservoirs of metal in the mantle and/or crust. It is unknown whether a large-scale metallic core, not represented by known meteorite samples, also formed on the same parent planetesimal. We can search for evidence of a molten, advecting core by assessing whether IIE irons contain remanent magnetization produced by a core dynamo. With this goal, we studied the paleomagnetism of a cloudy zone (CZ) interface in the Fe-Ni matrix of the IIE iron Colomera using X-ray photoelectron emission microscopy (XPEEM). Our initial results suggest that a steady, intense magnetic field was present during the gradual formation of the CZ. This may indicate the existence of an advecting core on the IIE parent body, which would support the hypothesis of a partially differentiated structure. We are continuing to test this conclusion with further XPEEM measurements on Colomera and other IIE irons.

Paleomagnetic Evidence for Partial Differentiation of the Silicate-Bearing IIE Iron Meteorite Parent Body

NASA Astrophysics Data System (ADS)

Maurel, C.; Bryson, J. F. J.; Weiss, B. P.; Scholl, A.

2017-12-01

The identification of dozens of petrologically diverse chondritic and achondritic meteoritic groups indicates that a diversity of planetesimals formed in the early solar system. It is commonly thought that planetesimals formed as either unmelted or else fully differentiated bodies, implying that chondrites and achondrites cannot have originated on a single body. However, it has been suggested that partially melted bodies with chondritic crusts and achondritic interiors may also have formed. This alternative proposal is supported by the recent identification of post-accretional remanent magnetization in CV, H chondrites, and also possibly in CM chondrites, which has been interpreted as possible evidence for a core dynamo on their parent bodies. Other piece of evidence suggesting the existence of partially differentiated bodies is the existence of the silicate-bearing IIE iron meteorites. The IIEs are composed of a Fe-Ni alloy matrix containing a mixture of chondritic, primitive achondritic, and chondritic silicate inclusions that likely formed on a single parent body. Therefore, IIEs may sample all three putative layers of a layered, partially differentiated body. On the other hand, the siderophile element compositions of the matrix metal demonstrate that it is not the product of fractional crystallization of a molten core. This suggests that the matrix metal is derived from isolated reservoirs of metal in the mantle and/or crust. It is unknown whether a large-scale metallic core, not represented by known meteorite samples, also formed on the same parent planetesimal. We can search for evidence of a molten, advecting core by assessing whether IIE irons contain remanent magnetization produced by a core dynamo. With this goal, we studied the paleomagnetism of a cloudy zone (CZ) interface in the Fe-Ni matrix of the IIE iron Colomera using X-ray photoelectron emission microscopy (XPEEM). Our initial results suggest that a steady, intense magnetic field was present during the gradual formation of the CZ. This may indicate the existence of an advecting core on the IIE parent body, which would support the hypothesis of a partially differentiated structure. We are continuing to test this conclusion with further XPEEM measurements on Colomera and other IIE irons.

Family-related predictors of body weight and weight-related behaviours among children and adolescents: a systematic umbrella review.

PubMed

Cislak, A; Safron, M; Pratt, M; Gaspar, T; Luszczynska, A

2012-05-01

This umbrella review analysed the relationships between family variables and child/adolescent body weight, diet and physical activity. In line with theories of health behaviour change, it was assumed that behaviour-specific family variables (i.e. beliefs, perceptions and practices referring to food intake or physical activity) would have stronger support than more general family variables (i.e. socio-economic status or general parental practices). Data obtained from 18 systematic reviews (examining 375 quantitative studies) were analysed. Reviews of experimental trials generally supported the effectiveness of reward/positive reinforcement parental strategies, parental involvement in treatment or prevention programmes, and cognitive-behavioural treatment in reducing child/adolescent body mass and/or obesity. Results across reviews of correlational studies indicated that healthy nutrition of children/adolescents was related to only one parental practice (parental monitoring), but was associated with several behaviour-specific family variables (e.g. a lack of restrictive control over food choices, high intake of healthy foods and low intake of unhealthy foods by parents and siblings, low pressure to consume foods). With regard to adolescent physical activity, stronger support was also found for behaviour-specific variables (e.g. physical activity of siblings), and for certain socio-economic variables (e.g. parental education). Child and adolescent obesity prevention programmes should account for behaviour-specific family variables. © 2011 Blackwell Publishing Ltd.

Authoritative feeding behaviors to reduce child BMI through online interventions.

PubMed

Frenn, Marilyn; Pruszynski, Jessica E; Felzer, Holly; Zhang, Jiannan

2013-01-01

PURPOSE.: The purpose of the study was to examine the feasibility and initial efficacies of parent- and/or child-focused online interventions and variables correlated with child body mass index percentile change. DESIGN AND METHODS.: A feasibility and cluster randomized controlled pilot study was used. RESULTS.: Recruitment was more effective at parent-teacher conferences compared with when materials were sent home with fifth- to eighth-grade culturally diverse students. Retention was 90% for students and 62-74% for parents. Authoritative parent feeding behaviors were associated with lower child body mass index. A larger study is warranted. PRACTICE IMPLICATIONS.: Online approaches may provide a feasible option for childhood obesity prevention and amelioration. © 2013, Wiley Periodicals, Inc.

Cosmogenic Effects in Bouvante Eucrite

NASA Astrophysics Data System (ADS)

Bhandari, N.; Bonino, G.; Cini Castagnoli, G.

1992-07-01

The Bouvante meteorite, a single stone weighing 8.3 kg, was found on 30th July 1978 and has been classified as a mononict recrystallized eucrite by Michel Levy et al. (1987). Here are the results of measurements of cosmic ray track density and radioisotopes ^26Al, ^22Na, and ^44Ti in a 700-g fragment taken from the main mass. Track Density: Four samples for track density measurements were taken from the farthest corners of the 700-g fragment and feldspars were etched in boiling 1:2 NaOH for 60 minutes. Track density in different fragments ranged between 3.1 X 10^4 to 2.7 X 10^5 tracks/cm^2 showing some gradient within the fragment. The exposure age of Bouvante has been determined from ^21,22Ne and other rare gases that yield values between 5.6 and 6.7 Ma (Weber et al., 1983). Adopting a value of 6 Ma leads to track production rate of 5 X 10^3 to 4.5 X 10^4 tracks/cm^2 Ma corresponding to ablation ranging between about 18 and 9 cm. If the mean value of 13.5 cm is taken as representative ablation then Bouvante had a pre-atmospheric radius of ~21 cm. Cosmogenic Radionuclides: Gamma ray emitters were measured by whole-rock counting with a low background gamma-ray spectrometer. A high purity, 372 cm^3, coaxial Ge diode located within a 10-cm- thick active NaI(Tl) well scintillator in a 20-cm-thick lead shield, in the underground laboratory of Monte dei Cappuccini in Torino (Bonino et al., 1991) served as the gamma ray detector. The detector was used in two modes, in coincidence and in anticoincidence with the scintillator. The counting efficiency was determined by using the inherently present ^40K as an internal standard and by calibrating the detector at different energies. K in Bouvante is known to be 610 ppm (Michel Levy et al., 1987). The sensitivity and selectivity of the detector is high and the background extremely low so that, in addition to the long lived ^26Al, 48-yr ^44Ti which is produced at very low levels and 2.6-yr ^22Na could be measured even after lapse of more than 13 years of the fall of the meteorite. The measured activities, at the time the meteorite was found are ^26Al = 91.6+-0.7 dpm/kg, ^22Na = 76.0+-7 dpm/kg and ^44Ti = 2.1+-0.5 dpm/kg. Upper limits of 0.8 dpm/kg were obtained for ^60Co and of 0.05 dpm/kg for ^42Ar. Uranium also could be estimated via its daughter ^214Bi to be ~200 ppb. The results could be compared with activities in another eucrite Bereba where a 400-g fragment was counted in a similar manner. The track density and the low ^60Co activity suggests that the meteorite was exposed as a small body (R(sub)pre ~=21 cm) in space. Measured activity of ^22Na is close to the expected value, when corrected for solar cycle modulation, and indicates that the meteorite did not fall much before the time it was found. We are grateful to Drs. P. Pellas and B. Zanda of the Muse de History Naturelle, Paris, for loaning us the Bouvante and Bereba meteorites. We thank Mr. K. M. Suthar for assistance in track analysis. References: Bonino G., Cini Castagnoli G., and Bhandari N. (1991) Il Nuovo Cimento (1991) (submitted); Michel Levy C., Bourot Denise M., Palme H., Spettel B., and Wanke H. (1987) Bull. Mineral., 110, 449; Weber H. W., Braun O., Schultz L., and Begemann F. (1983) Z. Naturforsch, 38a, 267.

School-based Parents' Groups--A Politics of Voice and Representation?

ERIC Educational Resources Information Center

Vincent, Carol; Martin, Jane

2000-01-01

Considers discussion-based parents' forums at two British secondary schools. Each school has attracted an elite group of white, middle-class professional women with limited decision-making power that remains unconnected to the wider parent body. It is difficult for controversial parental issues to be heard. (Contains 39 references.) (MLH)

Self-Esteem and Body Dissatisfaction in Young Children: Associations with Weight and Perceived Parenting Style

ERIC Educational Resources Information Center

Taylor, Amanda; Wilson, Carlene; Slater, Amy; Mohr, Philip

2012-01-01

Background: Parenting style has been associated with weight-related outcomes in children, but relationships between parenting, weight, and overweight-related psychological outcomes remain largely unstudied. The aim of the present study was to determine whether parenting was a moderator of the relationship between overweight and psychological…

Parental Management of Peer Relationships and Early Adolescents' Social Skills

ERIC Educational Resources Information Center

Mounts, Nina S.

2011-01-01

Despite a growing body of research on parental management of peer relationships, little is known about the relationship between parental management of peers and early adolescents' social skills or the precursors to parental management of peer relationships. The goals of this short-term longitudinal investigation were to examine the relationship…

DOE Office of Scientific and Technical Information (OSTI.GOV)

Vernazza, P.; Barge, P.; Zanda, B.

Although petrologic, chemical, and isotopic studies of ordinary chondrites and meteorites in general have largely helped establish a chronology of the earliest events of planetesimal formation and their evolution, there are several questions that cannot be resolved via laboratory measurements and/or experiments alone. Here, we propose the rationale for several new constraints on the formation and evolution of ordinary chondrite parent bodies (and, by extension, most planetesimals) from newly available spectral measurements and mineralogical analysis of main-belt S-type asteroids (83 objects) and unequilibrated ordinary chondrite meteorites (53 samples). Based on the latter, we suggest that spectral data may be usedmore » to distinguish whether an ordinary chondrite was formed near the surface or in the interior of its parent body. If these constraints are correct, the suggested implications include that: (1) large groups of compositionally similar asteroids are a natural outcome of planetesimal formation and, consequently, meteorites within a given class can originate from multiple parent bodies; (2) the surfaces of large (up to ∼200 km) S-type main-belt asteroids mostly expose the interiors of the primordial bodies, a likely consequence of impacts by small asteroids (D < 10 km) in the early solar system; (3) the duration of accretion of the H chondrite parent bodies was likely short (instantaneous or in less than ∼10{sup 5} yr, but certainly not as long as 1 Myr); (4) LL-like bodies formed closer to the Sun than H-like bodies, a possible consequence of the radial mixing and size sorting of chondrules in the protoplanetary disk prior to accretion.« less

Evidence for a Heterogeneous Distribution of Water in the Martian Interior

NASA Technical Reports Server (NTRS)

McCubbin, Francis; Boyce, Jeremy W.; Srinvasan, Poorna; Santos, Alison R.; Elardo, Stephen M.; Filiberto, Justin; Steele, Andrew; Shearer, Charles K.

2016-01-01

The abundance and distribution of H2O within the terrestrial planets, as well as its timing of delivery, is a topic of vital importance for understanding the chemical and physical evolution of planets and their potential for hosting habitable environments. Analysis of planetary materials from Mars, the Moon, and the eucrite parent body (i.e., asteroid 4Vesta) have confirmed the presence of H2O within their interiors. Moreover, H and N isotopic data from these planetary materials suggests H2O was delivered to the inner solar system very early from a common source, similar in composition to the carbonaceous chondrites. Despite the ubiquity of H2O in the inner Solar System, the only destination with any prospects for past or present habitable environments at this time, outside of the Earth, is Mars. Although the presence of H2O within the martian interior has been confirmed, very little is known regarding its abundance and distribution within the martian interior and how the martian water inventory has changed over time. By combining new analyses of martian apatites within a large number of martian meteorite types with previously published volatile data and recently determined mineral-melt partition coefficients for apatite, we report new insights into the abundance and distribution of volatiles in the martian crust and mantle. Using the subset of samples that did not exhibit crustal contamination, we determined that the enriched shergottite mantle source has 36-73 ppm H2O and the depleted shergottite mantle source has 14-23 ppm H2O. This result is consistent with other observed geochemical differences between enriched and depleted shergottites and supports the idea that there are at least two geochemically distinct reservoirs in the martian mantle. We also estimated the H2O content of the martian crust using the revised mantle H2O abundances and known crust-mantle distributions of incompatible lithophile elements. We determined that the bulk martian crust has approximately 1400 ppm H2O, which is likely distributed toward the martian surface. This crustal water abundance would equate to a global equivalent layer (GEL) of water at a depth of-229 m, which can account for at least some of the surface features on Mars attributed to flowing water and may be sufficient to support the past presence of a shallow sea on Mars' surface.

Paris vs. Murchison: Impact of hydrothermal alteration on organic matter in CM chondrites

NASA Astrophysics Data System (ADS)

Vinogradoff, V.; Le Guillou, C.; Bernard, S.; Binet, L.; Cartigny, P.; Brearley, A. J.; Remusat, L.

2017-09-01

Unravelling the origin of organic compounds that were accreted into asteroids requires better constraining the impact of asteroidal hydrothermal alteration on their isotopic signatures, molecular structures, and spatial distribution. Here, we conducted a multi-scale/multi-technique comparative study of the organic matter (OM) from two CM chondrites (that originate from the same parent body or from identical parent bodies that accreted the same mixture of precursors) and underwent a different degree of hydrothermal alteration: Paris (a weakly altered CM chondrite - CM 2.8) and Murchison (a more altered one - CM 2.5). The Paris insoluble organic matter (IOM) shows a higher aliphatic/aromatic carbon ratio, a higher radical abundance and a lower oxygen content than the Murchison IOM. Analysis of the OM in situ shows that two texturally distinct populations of organic compounds are present within the Paris matrix: sub-micrometric individual OM particles and diffuse OM finely distributed within phyllosilicates and amorphous silicates. These results indicate that hydrothermal alteration on the CM parent body induced aromatization and oxidation of the IOM, as well as a decrease in radical and nitrogen contents. Some of these observations were also reported by studies of variably altered fragment of Tagish Lake (C2), although the hydrothermal alteration of the OM in Tagish Lake was apparently much more severe. Finally, comparison with data available in the literature suggests that the parent bodies of other chondrite petrologic groups could have accreted a mixture of organic precursors different from that accreted by the parent body of CMs.

Caregivers feeding styles questionnaire. Establishing cutoff points

USDA-ARS?s Scientific Manuscript database

Researchers use the Caregiver's Feeding Styles Questionnaire (CFSQ) to categorize parent feeding into authoritative, authoritarian, indulgent, and uninvolved styles. The CFSQ assesses self-reported feeding and classifies parents using median splits which are used in a substantial body of parenting l...

Polar body biopsy in the diagnosis of monogenic diseases: the birth of three healthy children.

PubMed

Griesinger, Georg; Bündgen, Nana; Salmen, Diana; Schwinger, Eberhard; Gillessen-Kaesbach, Gabriele; Diedrich, Klaus

2009-08-01

For prospective parents at risk of transmitting a monogenic disease, polar body analysis is an option for pre-conception genetic diagnosis. In Germany, polar body analysis is currently performed in only two centers (Lübeck and Regensburg). The authors present a clinical series of 9 couples at risk for the transmission of a monogenic disease who underwent in vitro fertilization with polar body analysis. Nine couples have undergone in vitro fertilization with polar body analysis at the center in Lübeck since 2004. Three healthy children were born after polar body analysis for mucopolysaccharidosis type I, incontinentia pigmenti, and cystic fibrosis. The decision to undergo in vitro fertilization with polar body analysis is not easy for prospective parents to take, even though it often follows years of emotional suffering. Treatment with the methods of reproductive medicine in general, and with polar body analysis in particular, can cause considerable physical and emotional stress. For prospective parents in Germany at risk of transmitting a monogenic disease, polar body-based preimplantation diagnosis is an alternative to prenatal diagnosis and possible termination of pregnancy. The live birth rate per treatment cycle in this clinical series was 30%, which can be considered satisfactory. Nonetheless, most of the couples who did not achieve pregnancy after a first treatment cycle dropped out of treatment prematurely and did not go on to a second cycle.

The Longitudinal Causal Directionality between Body Image Distress and Self-Esteem among Korean Adolescents: The Moderating Effect of Relationships with Parents

ERIC Educational Resources Information Center

Park, Woochul; Epstein, Norman B.

2013-01-01

This study examined the longitudinal relationship between self-esteem and body image distress, as well as the moderating effect of relationships with parents, among adolescents in Korea, using nationally representative prospective panel data. Regarding causal direction, the findings supported bi-directionality for girls, but for boys the…

Principals' Perceptions and Experiences of the Role Parents Play in School Governing Bodies in Rural Areas

ERIC Educational Resources Information Center

Hartell, Cycil; Dippenaar, Hanlie; Moen, Melanie; Dladla, Themba

2016-01-01

This study investigated the perceptions and experiences of rural school principals in South Africa of the role that parents in the school governing bodies (SGBs) play in improving school management and governance. The study reports on a literature review as well as on the empirical investigation, which was based on a qualitative research paradigm.…

Talking Relationships, Babies and Bodies with Young Children: The Experiences of Parents in England

ERIC Educational Resources Information Center

Stone, Nicole; Ingham, Roger; McGinn, Laura; Bengry-Howell, Andrew

2017-01-01

Parents often find themselves ill-prepared for the moment at which questions of a sexual nature arise, or when children display signs of playful behaviour that can be interpreted as sexual. How these behaviours and questions are dealt with establishes the foundations on which children begin to interpret relationships, their bodies, those of others…

Early aqueous activity on the ordinary and carbonaceous chondrite parent bodies recorded by fayalite

DOE Office of Scientific and Technical Information (OSTI.GOV)

Doyle, Patricia M.; Jogo, Kaori; Nagashima, Kazuhide

Here, chronology of aqueous activity on chondrite parent bodies constrains their accretion times and thermal histories. Radiometric 53Mn– 53Cr dating has been successfully applied to aqueously formed carbonates in CM carbonaceous chondrites. Owing to the absence of carbonates in ordinary (H, L and LL), and CV and CO carbonaceous chondrites, and the lack of proper standards, there are no reliable ages of aqueous activity on their parent bodies. Here we report the first 53Mn– 53Cr ages of aqueously formed fayalite in the L3 chondrite Elephant Moraine 90161 as 2.4 +1.8 -1.3 Myr after calcium–aluminium-rich inclusions (CAIs), the oldest Solar Systemmore » solids. In addition, measurements using our synthesized fayalite standard show that fayalite in the CV3 chondrite Asuka 881317 and CO3-like chondrite MacAlpine Hills 88107 formed and 4.2 +0.8 -0.7 Myr after CAIs, respectively. Thermal modelling, combined with the inferred conditions (temperature and water/rock ratio) and 53Mn– 53Cr ages of aqueous alteration, suggests accretion of the L, CV and CO parent bodies ~1.8–2.5 Myr after CAIs.« less

Early aqueous activity on the ordinary and carbonaceous chondrite parent bodies recorded by fayalite

DOE PAGES

Doyle, Patricia M.; Jogo, Kaori; Nagashima, Kazuhide; ...

2015-06-23

Here, chronology of aqueous activity on chondrite parent bodies constrains their accretion times and thermal histories. Radiometric 53Mn– 53Cr dating has been successfully applied to aqueously formed carbonates in CM carbonaceous chondrites. Owing to the absence of carbonates in ordinary (H, L and LL), and CV and CO carbonaceous chondrites, and the lack of proper standards, there are no reliable ages of aqueous activity on their parent bodies. Here we report the first 53Mn– 53Cr ages of aqueously formed fayalite in the L3 chondrite Elephant Moraine 90161 as 2.4 +1.8 -1.3 Myr after calcium–aluminium-rich inclusions (CAIs), the oldest Solar Systemmore » solids. In addition, measurements using our synthesized fayalite standard show that fayalite in the CV3 chondrite Asuka 881317 and CO3-like chondrite MacAlpine Hills 88107 formed and 4.2 +0.8 -0.7 Myr after CAIs, respectively. Thermal modelling, combined with the inferred conditions (temperature and water/rock ratio) and 53Mn– 53Cr ages of aqueous alteration, suggests accretion of the L, CV and CO parent bodies ~1.8–2.5 Myr after CAIs.« less

Ar-Ar and I-Xe Ages of Caddo County and Thermal History of IAB Iron Meteorites

NASA Technical Reports Server (NTRS)

Bogard, Donald D.; Garrison, Daniel H.; Takeda, Hiroshi

2005-01-01

Inclusions in IAB iron meteorites include non-chondritic silicate and those with more primitive chondritic silicate composition. Coarse-grained gabbroic material rich in plagioclase and diopside occurs in the Caddo County IAB iron meteorite and represents a new type of chemically differentiated, extra-terrestrial, andesitic silicate. Other parts of Caddo contain mostly andesitic material. Caddo thus exhibits petrologic characteristics of parent body metamorphism of a chondrite-like parent and inhomogeneous segregation of melts. Proposed IAB formation models include parent body partial melting and fractional crystallization or incomplete differentiation due to internal heat sources, and impact/induced melting and mixing. Benedix et al. prefer a hybrid model whereby the IAB parent body largely melted, then underwent collisional breakup, partial mixing of phases, and reassembly. Most reported 129I- Xe-129 ages of IABs are greater than 4.56 Gyr and a few are greater than or = 4.567 Gyr. These oldest ages exceed the 4.567 Gyr Pb-Pb age of Ca, Al-rich inclusions in primitive meteorites,

Nature of the H chondrite parent body regolith - Evidence from the Dimmitt breccia

NASA Technical Reports Server (NTRS)

Rubin, A. E.; Scott, E. R. D.; Taylor, G. J.; Keil, K.; Allen, J. S. B.; Mayeda, T. K.; Clayton, R. N.; Bogard, D. D.

1983-01-01

Meteorite regolith breccias are clastic rocks which formed by lithification of fragmental regolith material that once resided at the surface of a meteorite parent body. A study is reported of the matrix and 21 clasts of various sizes (0.2-24 mm) in the Dimmitt H chondrite regolith breccia using petrographic and electron microprobe techniques. In addition, oxygen isotope studies of three clasts and instrumental neutron activation analysis (INAA) and Ar-39/Ar-40 age dating of one clast are reported. The Dimmitt meteorite was found about 1942 near Dimmitt, Texas. Attention is given to analytical procedures, the clastic matrix, equilibrated clasts, poikilitic melt-rock clast, clasts of different chondrite groups, graphite-magnetite aggregates, the origin of exotic clasts, and the complexity of parent body surfaces processes.

Space Weathering of Ordinary Chondrite Parent Bodies, Its Impact on the Method of Distinguishing H, L, and LL Types and Implications for Itokawa Samples Returned by the Hayabusa Mission

NASA Technical Reports Server (NTRS)

Hiroi, T.; Sasaki, S.; Noble, S. K.; Pieters, C. M.

2011-01-01

As the most abundance meteorites in our collections, ordinary chondrites potentially have very important implications on the origin and formation of our Solar System. In order to map the distribution of ordinary chondrite-like asteroids through remote sensing, the space weathering effects of ordinary chondrite parent bodies must be addressed through experiments and modeling. Of particular importance is the impact on distinguishing different types (H/L/LL) of ordinary chondrites. In addition, samples of asteroid Itokawa returned by the Hayabusa spacecraft may re veal the mechanism of space weathering on an LLchondrite parent body. Results of space weathering simulations on ordinary chondrites and implications for Itokawa samples are presented here.

Gay and Lesbian Parents

MedlinePlus

... Life Listen Español Text Size Email Print Share Gay and Lesbian Parents Page Content Article Body I am gay. Should I worry how this will affect my children? Millions of children have one or more gay and/or lesbian parents. For some children, having ...

Body Talk for Parents of Girls.

ERIC Educational Resources Information Center

Stubbs, Margaret L.

This pamphlet, targeted to girls' parents, discusses issues surrounding puberty. The introduction discusses cultural images of menstruation and girls' attitudes towards it. Suggestions are offered for discussing menstruation with one's daughter. Suggestions focus on timing of introducing the topic; which parent takes responsibility for menstrual…

Children's Eating Attitudes and Behaviour: A Study of the Modelling and Control Theories of Parental Influence

ERIC Educational Resources Information Center

Brown, Rachael; Ogden, Jane

2004-01-01

The present study compared the modelling and control theories of parental influence on children's eating attitudes and behaviour with a focus on snack foods. Matched questionnaires describing reported snack intake, eating motivations and body dissatisfaction were completed by 112 parent/child pairs. Parents completed additional items relating to…

The Role of Parents in Young People's Education--A Critical Review of the Causal Evidence

ERIC Educational Resources Information Center

See, Beng Huat; Gorard, Stephen

2015-01-01

There is currently a considerable body of research suggesting that parental involvement is linked to young people's attainment at school. It is also generally agreed that a number of factors such as parental background, attention, warmth and parenting style are associated with children's later life outcomes. However, although widely assumed on the…

Parental Belief and Parental Engagement: How Do They Interact?

ERIC Educational Resources Information Center

Goodall, Janet

2013-01-01

Previous literature has shown the importance of parental engagement for children's outcomes; a largely separate body of literature has shown that there are clear effects on children's outcomes related to parental religion. This article is a literature review of these two fields, with the aim of relating them to each other. The article suggests two…

Parents' Perceptions of Children's Weight: The Accuracy of Ratings and Associations to Strategies for Feeding

ERIC Educational Resources Information Center

Tremblay, Line; Rinaldi, Christina M.; Lovsin, Tanya; Zecevic, Cheryl

2012-01-01

The general objective of this study was to assess parents' perceptions of their preschooler's body weight, and the association between children's current weight status and parental feeding strategies. A sample of 150 parents of three- to five-year-old children (72 girls and 78 boys) completed questionnaires on sociodemographic information,…

Parental history of hypertension is associated with narrower retinal arteriolar caliber in young girls.

PubMed

Gopinath, Bamini; Baur, Louise A; Hardy, Louise L; Wang, Jie Jin; Teber, Erdahl; Wong, Tien Y; Mitchell, Paul

2011-09-01

We aimed to assess the associations between parental history of hypertension and indicators of cardiovascular risk (retinal vessel diameter, presence of obesity, and elevated blood pressure) in prepubertal children. There were 1739 (77.7% of those eligible) 6-year-old students (863 girls and 876 boys) who were examined from a random cluster sample of 34 Sydney schools. Parents completed questionnaires about their medical conditions, including whether they have/had hypertension. Retinal images were taken with a digital fundus camera, and retinal vessel caliber was quantified using computer software. Anthropometric (height, weight, percentage of body fat, and body mass index) and blood pressure measures were collected. There were 160 children (9.2%) with a positive parental history of hypertension (either biological mother and/or father). Children with a positive versus negative parental history of hypertension had significantly higher body mass index (16.8 versus 16.5 kg/m(2); P=0.04) and systolic blood pressure (101.3 versus 99.8 mm Hg; P=0.01). Girls with positive versus negative parental history of hypertension had significantly higher diastolic blood pressure (≈3.1 mm Hg; P=0.01) and narrower retinal arteriolar caliber (≈4.3 μm; P=0.0004). Positive parental history of hypertension was not associated with mean retinal vascular caliber among boys. We show that a positive parental history of hypertension in healthy prepubertal girls, but not boys, is associated with narrower retinal arteriolar vessels, likely conveying a predisposition to develop hypertension later in life. These findings may indicate the need for cardiovascular disease prevention measures starting early in life among offspring of hypertensive parents.

Parental and Child Characteristics Related to Early-Onset Disordered Eating: A Systematic Review.

PubMed

Larsen, Pernille Stemann; Strandberg-Larsen, Katrine; Micali, Nadia; Andersen, Anne-Marie Nybo

2015-01-01

After participating in this activity, learners should be better able to: Evaluate the evidence regarding parental and child characteristics related to early-onset disordered eating. Eating disorders are rare in children, but disordered eating is common. Understanding the phenomenology of disordered eating in childhood can aid prevention of full-blown eating disorders. The purpose of this review is to systematically extract and synthesize the evidence on parental and child characteristics related to early-onset disordered eating. Systematic searches were conducted in PubMED/MEDLINE, EMBASE, and PsycInfo using the following search terms: eating disorder, disordered eating, problem eating, anorexia nervosa, bulimia nervosa, binge eating, child, preadolescent, and early onset. Studies published from 1990 to 2013 addressing parental and child characteristics of disordered eating in children aged 6 to 12 years were eligible for inclusion. The search was restricted to studies with cross-sectional, case-control, or longitudinal designs, studies in English, and with abstracts available. Forty-four studies fit these criteria. Most studies were based on community samples with a cross-sectional design. The included studies varied considerably in size, instruments used to assess early-onset disordered eating, and parental and child characteristics investigated. Important determinants included the following: higher body weight, previously reported disordered eating, body dissatisfaction, depression, parental disordered eating, and parental comments/concerns about child's weight and eating. The findings were inconsistent for sex, age, socioeconomic status, ethnicity, self-esteem/worth, and parental body weight. In conclusion, characteristics related to early-onset disordered eating have mainly been explored with a cross-sectional design. Full understanding of causal pathways will require good-quality longitudinal studies designed to address the influence of parental eating behaviors, mental and physical health, family interactions, and child growth patterns.

Parental bonds, attachment anxiety, media susceptibility, and body dissatisfaction: a mediation model.

PubMed

Patton, Sarah C; Beaujean, A Alexander; Benedict, Helen E

2014-08-01

The developmental trajectory of body image dissatisfaction is unclear. Researchers have investigated sociocultural and developmental risk factors; however, the literature needs an integrative etiological model. In 2009, Cheng and Mallinckrodt proposed a dual mediation model, positing that poor-quality parental bonds, via the mechanisms of heightening romantic attachment anxiety and thin-ideal media internalization, increases body dissatisfaction. We tested 2 versions of this model, including an alternate model featuring attachment anxiety in close friendships. We recruited females ages 12-24, primarily from a mid-sized private religious university, to complete self-report measures. The participant sample was ethnically diverse, with approximately 40% endorsing minority status. Results showed that mother care and father care were negatively linked to friendship attachment anxiety and romantic attachment anxiety. Friendship and romantic attachment anxiety were positively linked to media susceptibility. Media susceptibility was positively linked to body image dissatisfaction. Mother care and father care were negatively, indirectly linked to body image dissatisfaction through the mediators of friendship attachment anxiety and media susceptibility. Mother care made a significant, albeit small, contribution to body image dissatisfaction after controlling for other variables. Overall, findings suggest that adverse parent-child relational factors may indirectly elevate body dissatisfaction, operating through attachment anxiety and susceptibility to sociocultural pressures. PsycINFO Database Record (c) 2014 APA, all rights reserved.

Perceptions of early body image socialization in families: Exploring knowledge, beliefs, and strategies among mothers of preschoolers.

PubMed

Liechty, Janet M; Clarke, Samantha; Birky, Julie P; Harrison, Kristen

2016-12-01

This study sought to explore parental perceptions of body image in preschoolers. We conducted semi-structured interviews with 30 primary caregivers of preschoolers to examine knowledge, beliefs, and strategies regarding early body image socialization in families. Thematic Analysis yielded three themes highlighting knowledge gaps, belief discrepancies, and limited awareness of strategies. Findings regarding knowledge: Most participants defined body image as objective attractiveness rather than subjective self-assessment (53%) and focused on negative body image. Beliefs: Although 97% of participants believed weight and shape impact children's self-esteem, 63% believed preschoolers too young to have a body image. Strategies: Most participants (53%) said family was a primary influence on body image, but identified few effective strategies and 63% said they did not do anything to influence children's body image. Findings suggested family body image socialization in preschoolers is occurring outside the awareness of parents and the concept of positive body image is underdeveloped. Copyright © 2016 Elsevier Ltd. All rights reserved.

Brood desertion by female shorebirds: a test of the differential parental capacity hypothesis on Kentish plovers.

PubMed Central

Amat, J A; Visser, G H; Pérez-Hurtado, A; Arroyo, G M

2000-01-01

The aim of this study was to examine whether the energetic costs of reproduction explain offspring desertion by female shorebirds, as is suggested by the differential parental capacity hypothesis. A prediction of the hypothesis is that, in species with biparental incubation in which females desert from brood care after hatching, the body condition of females should decline after laying to a point at which their body reserves are too low for continuing parental care. We tested this prediction on Kentish plovers (Charadrius alexandrinus) in which both sexes incubate but the females desert from brood care before the chicks fledge. We found no changes in either the body masses or body compositions of both individual male and female plovers from early incubation and throughout early chick rearing. Furthermore, the timing of brood desertion by females was not affected by their body condition. Neither did we find gender differences in the energetic costs of incubation. There were no differences in the timing of brood desertion between experimental and control females in an experiment in which we lengthened or shortened the duration of incubation by one week. These results indicate that energetic costs do not explain offspring desertion by female Kentish plovers and that the needs of chicks for parental care rather than cumulative investment by females is what determines the timing of brood desertion. PMID:11413629

Impact simulation in the gravity regime: Exploring the effects of parent body size and internal structure

NASA Astrophysics Data System (ADS)

Benavidez, P. G.; Durda, D. D.; Enke, B.; Campo Bagatin, A.; Richardson, D. C.; Asphaug, E.; Bottke, W. F.

2018-04-01

In this work we extend the systematic investigation of impact outcomes of 100-km-diameter targets started by Durda et al. (2007) and Benavidez et al. (2012) to targets of D = 400 km using the same range of impact conditions and two internal structures: monolithic and rubble-pile. We performed a new set of simulations in the gravity regime for targets of 400 km in diameter using these same internal structures. This provides a large set of 600 simulations performed in a systematic way that permits a thorough analysis of the impact outcomes and evaluation of the main features of the size frequency distribution due mostly to self-gravity. In addition, we use the impact outcomes to attempt to constrain the impact conditions of the asteroid belt where known asteroid families with a large expected parent body were formed. We have found fairly good matches for the Eunomia and Hygiea families. In addition, we identified a potential acceptable match to the Vesta family from a monolithic parent body of 468 km. The impact conditions of the best matches suggest that these families were formed in a dynamically excited belt. The results also suggest that the parent body of the Eunomia family could be a monolithic body of 382 km diameter, while the one for Hygiea could have a rubble-pile internal structure of 416 km diameter.

Effect of parental age and associated size on fecundity, growth and survival in the yellow seahorse Hippocampus kuda.

PubMed

Dzyuba, Borys; Van Look, Katrien J W; Cliffe, Alex; Koldewey, Heather J; Holt, William V

2006-08-01

Seahorses, together with the pipefishes (Family Syngnathidae), are the only vertebrates in which embryonic development takes place within a specialised body compartment, the brood pouch, of the male instead of the female. Embryos develop in close association with the brood pouch epithelium in a manner that bears some resemblance to embryo-placental relationships in mammals. We have explored the hypothesis that parental body size and age should affect offspring postnatal growth and survival if brood pouch quality impacts upon prenatal embryonic nutrition or respiration. Using an aquarium population of the yellow seahorse, Hippocampus kuda, we show here that large parents produce offspring whose initial postnatal growth rates (weeks one to three) were significantly higher than those of the offspring of younger and smaller parents. Whereas 90% of offspring from the larger parents survived for the duration of the study (7 weeks), less that 50% of offspring from smaller parents survived for the same period. For the offspring of large parents, growth rates from individual males were negatively correlated with the number of offspring in the cohort (r=-0.82; P<0.05); this was not the case for offspring from small parents (r=0.048; P>0.9). Observations of embryos within the pouch suggested that when relatively few embryos are present they may attach to functionally advantageous sites and thus gain physiological support during gestation. These results suggest that male body size, and pouch size and function, may influence the future fitness and survival of their offspring.

Flexibility in the parental effort of an Arctic-breeding seabird

USGS Publications Warehouse

Harding, A.M.A.; Kitaysky, A.S.; Hall, M.E.; Welcker, J.; Karnovsky, N.J.; Talbot, S.L.; Hamer, K.C.; Gremillet, D.

2009-01-01

Parental investment strategies are considered to represent a trade-off between the benefits of investment in current offspring and costs to future reproduction. Due to their high residual reproductive value, long-lived organisms are predicted to be more reluctant to increase parental effort. 2. We tested the hypothesis that breeding little auks (Alle alle) have a fixed level of reproductive investment, and thus reduce parental effort when costs associated with reproduction increase. 3. To test this hypothesis we experimentally increased the flight costs of breeding little auks via feather clipping. In 2005 we examined changes in the condition of manipulated parents, of the mates of manipulated parents, and of their chick as direct measures of change in parental resource allocation between self-maintenance and current reproduction. In 2007 we increased sample sizes to determine whether there was a physiological cost (elevated corticosterone, CORT) associated with the manipulation. 4. We found that: (i) clipped birds and their mates lost more body mass than controls, but there was no difference in mass loss between members of a pair; (ii) clipped birds had higher CORT levels than control birds; (iii) there were no inter-annual differences in body mass and CORT levels between clipped individuals and their mates at recapture, and (iv) chicks with a clipped parent had lower peak and fledging mass, and higher CORT levels than control chicks in both years. 5. Contrary to our hypothesis, the reduction in body mass of partners to clipped birds suggests that little auks can increase parental effort to some extent. Nonetheless, the lower fledging mass and higher CORT of chicks with a clipped parent indicates provisioning rates may not have been fully maintained. 6. As predicted by life-history theory, there may be a threshold to the additional reproductive costs breeders will accept, with parents prioritizing self-maintenance over increased provisioning effort when foraging costs become too high. ?? 2008 British Ecological Society.

Female patients' and parents' assessment of deformity- and brace-related stress in the conservative treatment of adolescent idiopathic scoliosis.

PubMed

Misterska, Ewa; Glowacki, Maciej; Latuszewska, Joanna

2012-06-15

A cross-sectional analysis of parents' and patients' perceptions of deformity- and brace-related stress regarding conservative treatment of adolescent idiopathic scoliosis. The purpose of this study was to determine the agreement between patients' and parents' assessments of emotional stress and to compare these assessments with radiographical measurements of spinal deformity. Conservative treatment in patients with scoliosis may cause emotional stress. To our knowledge, no group has ever reported patient and parental estimation of stress related to wearing a brace and spinal deformity in girls with adolescent idiopathic scoliosis. Sixty-three pairs of parents and girls with adolescent idiopathic scoliosis treated with a Cheneau brace were separately asked to complete the Bad Sobberheim Stress Questionnaire-Deformity and the Bad Sobberheim Stress Questionnaire-Brace. The age range of the patients was from 10 to 17 years. Patients were assessed at a mean of 14.12 (SD, 10.99) months after the start of the conservative treatment. Patients thought that a moderate level of stress was connected with conservative treatment; however, the stress level, related to perceived trunk deformation, was low. From the parents' perspective, patients experienced a moderate level of stress during conservative treatment and related to spinal deformity. The study groups differ in their perception of stress levels due to body disfigurement but not during the conservative treatment. Parent-patient stress-level disparities were not related to body mass index, age of the patient, brace application, and radiographical measurements of spinal deformity. Patients and parents perceive the emotional stress related to brace treatment in the same way; however, parents overestimate the assessment of stress levels related to body deformity. From the perspective of patients and parents, brace wearing increased the level of stress induced by the deformity alone. Complete assessment of conservative treatment should include evaluation of emotional stress from the perspective of patients and parents.

Body Talk for Parents of Boys.

ERIC Educational Resources Information Center

Stubbs, Margaret L.

This pamphlet, targeted to boys' parents, discusses issues surrounding puberty. The introduction discusses education about menstruation and girls' and boys' attitudes towards it. Suggestions are offered for discussing menstruation with one's son. Suggestions focus on timing of introducing the topic; which parent takes responsibility for menstrual…

Changes in Parent Motivation Predicts Changes in Body Mass Index z-Score (zBMI) and Dietary Intake Among Preschoolers Enrolled in a Family-Based Obesity Intervention

PubMed Central

Kuhl, Elizabeth S.; Filigno, Stephanie S.; Clifford, Lisa M.; Connor, Jared M.; Stark, Lori J.

2014-01-01

Objectives To examine whether changes in parent motivation over the course of a pediatric obesity intervention are significantly associated with long-term changes in treatment outcomes. Methods Study hypotheses were tested with a secondary data analysis of a randomized controlled trial (N = 42). Study analyses tested whether baseline to posttreatment change in total score for a self-report parent motivation measure (Parent Motivation Inventory [PMI]) was significantly associated with baseline to 6-month follow-up changes in body mass index z-score (zBMI), dietary variables, and physical activity. Results Increases in PMI were significantly associated with decreased zBMI, decreased consumption of sugar-sweetened beverages and sweets, and increased consumption of artificially sweetened beverages. Conclusions Given that increases in parent motivation were associated with some treatment benefits, future research should evaluate the impact of directly assessing and targeting parent motivation on weight outcomes for preschoolers participating in a weight management program. PMID:25016604

Facial and bodily correlates of family background.

PubMed

Boothroyd, Lynda G; Perrett, David I

2006-09-22

It has been suggested that absence of the father during early childhood has long-reaching effects on reproductive strategy and development of offspring. This paper reports two studies designed to investigate the physical characteristics of daughters associated with father absence. Study 1 used a facial averaging method to produce composite images of faces of women whose parents separated during their childhood (who were 'father absent'), women whose parents remained together, but had poor quality relationships and women whose parents were together and had good quality relationships. Images were then rated by male and female judges. Father absence and poor parental relationships were associated with apparent facial masculinity and reduced attractiveness in daughters. Poor parental relationships were also associated with reduced apparent health. Study 2 compared family background with body measurements and found that father absence or a poor quality relationship between parents were associated with body masculinity (high waist-to-hip ratio) and increased weight-for-height and adiposity. These results highlight the possibility of physical masculinization being associated with purported father absence 'effects'.

The Differing Amounts of Freedom Parents Allow Their Preschool Sons and Daughters to Discuss Body Self Concept.

ERIC Educational Resources Information Center

Story, Marilyn

Parents of all children in a university home economics department preschool (N=18), a university day care center (N=40), and a Montessori Method preschool (N=36) were contacted to determine if they allowed their preschool children differing amounts of freedom to discuss body self-concepts according to sex of the child or type of preschool the…

Relationship of Adherence Determinants and Parental Spirituality in Cystic Fibrosis

PubMed Central

Grossoehme, Daniel H.; Opipari-Arrigan, Lisa; VanDyke, Rhonda; Thurmond, Sophia; Seid, Michael

2015-01-01

Summary The course of cystic fibrosis (CF) progression in children is affected by parent adherence to treatment plans. The Theory of Reasoned Action (TRA) posits that intentions are the best behavioral predictors and that intentions reasonably follow from beliefs (“determinants”). Determinants are affected by multiple “background factors,” including spirituality. This study’s purpose was to understand whether two parental adherence determinants (attitude towards treatment and self-efficacy) were associated with spirituality (religious coping and sanctification of the body). We hypothesized that parents’ attitudes toward treatment adherence are associated with these spiritual constructs. A convenience sample of parents of children with CF aged 3–12 years (n = 28) participated by completing surveys of adherence and spirituality during a regular outpatient clinic visit. Type and degree of religious coping was examined using principal component analysis. Adherence measures were compared based on religious coping styles and sanctification of the body using unpaired t-tests. Collaborative religious coping was associated with higher self-efficacy for completing airway clearance (M = 1070.8; SD = 35.8; P = 0.012), for completing aerosolized medication administration (M = 1077.1; SD = 37.4; P = 0.018), and for attitude towards treatment utility (M = 38.8; SD = 2.36; P = 0.038). Parents who attributed sacred qualities to their child’s body (e.g., “blessed” or “miraculous”) had higher mean scores for self-efficacy (airway clearance, M = 1058.6; SD = 37.7; P = 0.023; aerosols M = 1070.8; SD = 41.6; P = 0.020). Parents for whom God was manifested in their child’s body (e.g., “My child’s body is created in God’s image”) had higher mean scores for self-efficacy for airway clearance (M = 1056.4; SD = 59.0; P = 0.039), aerosolized medications (M = 1068.8; SD = 42.6; P = 0.033) and treatment utility (M = 38.8; SD = 2.4; P = 0.025). Spiritual constructs show promising significance and are currently undervalued in chronic disease management. PMID:22170872

Relationship of adherence determinants and parental spirituality in cystic fibrosis.

PubMed

Grossoehme, Daniel H; Opipari-Arrigan, Lisa; VanDyke, Rhonda; Thurmond, Sophia; Seid, Michael

2012-06-01

The course of cystic fibrosis (CF) progression in children is affected by parent adherence to treatment plans. The Theory of Reasoned Action (TRA) posits that intentions are the best behavioral predictors and that intentions reasonably follow from beliefs ("determinants"). Determinants are affected by multiple "background factors," including spirituality. This study's purpose was to understand whether two parental adherence determinants (attitude towards treatment and self-efficacy) were associated with spirituality (religious coping and sanctification of the body). We hypothesized that parents' attitudes toward treatment adherence are associated with these spiritual constructs. A convenience sample of parents of children with CF aged 3-12 years (n = 28) participated by completing surveys of adherence and spirituality during a regular outpatient clinic visit. Type and degree of religious coping was examined using principal component analysis. Adherence measures were compared based on religious coping styles and sanctification of the body using unpaired t-tests. Collaborative religious coping was associated with higher self-efficacy for completing airway clearance (M = 1070.8; SD = 35.8; P = 0.012), for completing aerosolized medication administration (M = 1077.1; SD = 37.4; P = 0.018), and for attitude towards treatment utility (M = 38.8; SD = 2.36; P = 0.038). Parents who attributed sacred qualities to their child's body (e.g., "blessed" or "miraculous") had higher mean scores for self-efficacy (airway clearance, M = 1058.6; SD = 37.7; P = 0.023; aerosols M = 1070.8; SD = 41.6; P = 0.020). Parents for whom God was manifested in their child's body (e.g., "My child's body is created in God's image") had higher mean scores for self-efficacy for airway clearance (M = 1056.4; SD = 59.0; P = 0.039), aerosolized medications (M = 1068.8; SD = 42.6; P = 0.033) and treatment utility (M = 38.8; SD = 2.4; P = 0.025). Spiritual constructs show promising significance and are currently undervalued in chronic disease management. Copyright © 2011 Wiley Periodicals, Inc.

A new type of solar-system material recovered from Ordovician marine limestone

PubMed Central

Schmitz, B.; Yin, Q. -Z.; Sanborn, M. E.; Tassinari, M.; Caplan, C. E.; Huss, G. R.

2016-01-01

From mid-Ordovician ∼470 Myr-old limestone >100 fossil L-chondritic meteorites have been recovered, representing the markedly enhanced flux of meteorites to Earth following the breakup of the L-chondrite parent body. Recently one anomalous meteorite, Österplana 065 (Öst 65), was found in the same beds that yield L chondrites. The cosmic-ray exposure age of Öst 65 shows that it may be a fragment of the impactor that broke up the L-chondrite parent body. Here we show that in a chromium versus oxygen-isotope plot Öst 65 falls outside all fields encompassing the known meteorite types. This may be the first documented example of an ‘extinct' meteorite, that is, a meteorite type that does not fall on Earth today because its parent body has been consumed by collisions. The meteorites found on Earth today apparently do not give a full representation of the kind of bodies in the asteroid belt ∼500 Myr ago. PMID:27299793

A new type of solar-system material recovered from Ordovician marine limestone.

PubMed

Schmitz, B; Yin, Q-Z; Sanborn, M E; Tassinari, M; Caplan, C E; Huss, G R

2016-06-14

From mid-Ordovician ∼470 Myr-old limestone >100 fossil L-chondritic meteorites have been recovered, representing the markedly enhanced flux of meteorites to Earth following the breakup of the L-chondrite parent body. Recently one anomalous meteorite, Österplana 065 (Öst 65), was found in the same beds that yield L chondrites. The cosmic-ray exposure age of Öst 65 shows that it may be a fragment of the impactor that broke up the L-chondrite parent body. Here we show that in a chromium versus oxygen-isotope plot Öst 65 falls outside all fields encompassing the known meteorite types. This may be the first documented example of an 'extinct' meteorite, that is, a meteorite type that does not fall on Earth today because its parent body has been consumed by collisions. The meteorites found on Earth today apparently do not give a full representation of the kind of bodies in the asteroid belt ∼500 Myr ago.

A prospective study on the impact of peer and parental pressure on body dissatisfaction in adolescent girls and boys.

PubMed

Helfert, Susanne; Warschburger, Petra

2011-03-01

The current study explores the role of appearance-related social pressure regarding changes in body image in adolescent girls (n=236) and boys (n=193) over a 1-year-period. High school students aged 11-16 completed measures of body dissatisfaction (i.e., weight and muscle concerns) and appearance-related social pressure from peers and parents. Three aspects proved to be particularly crucial: Parental encouragement to control weight and shape was a strong predictor of weight concerns in boys and girls alike; influences of friends affected gender-specific body image concerns by leading to weight concerns in girls and muscle concerns in boys; finally appearance-based exclusion was a predictor of weight concerns in boys. The findings provide longitudinal evidence for the crucial impact of appearance-related social pressure and suggest that a detailed assessment of different types of social impacts can identify concrete targets for effective prevention and therapy for weight-related problems among adolescents. Copyright © 2011 Elsevier Ltd. All rights reserved.

NASA's Ground-Based Observing Campaigns of Rocket Bodies with the UKIRT and NASA ES-MCAT Telescopes

NASA Technical Reports Server (NTRS)

Lederer, Susan M.; Buckalew, Brent A.; Anz-Meador, Phillip; Cowardin, Heather M.; Frith, James M.; Matney, Mark

2017-01-01

Rocket bodies comprise a class of human-made space debris that are at the same time essential for launching every spacecraft from the Earth, but are also a significant source of debris both as intact objects, as well as fragmented debris. Unspent fuel has been long theorized as a potential cause of catastrophic rocket body break-ups. Given typical orbital speeds range from approximately 2-3 kilometers per second at Geosynchronous Orbit (GEO) and up to 15 kilometers per second in low Earth orbit (LEO), collisions with uncatalogued and undetected debris can also cause catastrophic breakups. Understanding break-ups is a necessary step in preventing them, and one key step in that process is to correlate and characterize daughter fragments with their parent bodies. Two very different methods include (1) conducting photometric surveys to correlate an object's motion and orbital elements to the parent body, and (2) characterizing what materials comprise the target to determine whether those materials are consistent with the parent body or like objects. With this in mind, photometric data were taken shortly after the breakup of one rocket body for short-term orbital studies, and a suite of spectral data were taken of rocket bodies that are fully intact to compare with debris, for characterization studies. Targets included Titan Transtage, Briz-M, and Ariane rocket bodies and debris. Spectra of each sub-class of rocket body were very similar within their rocket body type, but differed distinctly from one type to the next, supporting the effectiveness of this approach.

Parent Involvement Intervention in Developing Weight Management Skills for both Parents and Overweight/Obese Children.

PubMed

Kim, Hee Soon; Park, Jiyoung; Park, Kye-Yeong; Lee, Myung-Nam; Ham, Ok Kyung

2016-03-01

The purpose of the study was to evaluate a parent involvement intervention for childhood obesity intended to increase parents' skills in managing children's weight-related behavior and to improve child-parent relationships. Many studies reported on parental influence on childhood obesity, emphasizing parent involvement in prevention and management of childhood obesity. A randomized controlled trial was conducted. Forty-two parents of overweight/obese children were recruited from four cities and randomized to the experimental group or control group. The parental intervention was provided only to parents in the experimental group and consisted of weekly newsletters and text messages for a period of 5 weeks. Exercise classes and nutrition education were provided to all children. Lifestyle Behaviour Checklist and the Child-Parent Relationship Scale (CPRS) were used for measurement of parent outcome. For the child outcome, dietary self-efficacy, exercise frequency, and body mass index were measured. A mixed-design analysis of variance was performed with city location entered as a random effect. After the intervention, CPRS of parents and dietary self-efficacy of children showed an increase in the experimental group (p < .05). Intervention effects differed significantly according to the city location regarding the control efficacy of parents and dietary self-efficacy of children (p < .05). The results support the effectiveness of the parent involvement intervention in promoting child-parent relationship and dietary self-efficacy of children. However, a 5-week parent involvement intervention was not sufficient to produce significant changes in children's body mass index. Further research is needed to investigate effects of parent involvement intervention with long-term evaluation. Copyright © 2016. Published by Elsevier B.V.

Elephant Moraine 96029, a very mildly aqueously altered and heated CM carbonaceous chondrite: Implications for the drivers of parent body processing

NASA Astrophysics Data System (ADS)

Lee, Martin R.; Lindgren, Paula; King, Ashley J.; Greenwood, Richard C.; Franchi, Ian A.; Sparkes, Robert

2016-08-01

Elephant Moraine (EET) 96029 is a CM carbonaceous chondrite regolith breccia with evidence for unusually mild aqueous alteration, a later phase of heating and terrestrial weathering. The presence of phyllosilicates and carbonates within chondrules and the fine-grained matrix indicates that this meteorite was aqueously altered in its parent body. Features showing that water-mediated processing was arrested at a very early stage include a matrix with a low magnesium/iron ratio, chondrules whose mesostasis contains glass and/or quench crystallites, and a gehlenite-bearing calcium- and aluminium-rich inclusion. EET 96029 is also rich in Fe,Ni metal relative to other CM chondrites, and more was present prior to its partial replacement by goethite during Antarctic weathering. In combination, these properties indicate that EET 96029 is one of the least aqueously altered CMs yet described (CM2.7) and so provides new insights into the original composition of its parent body. Following aqueous alteration, and whilst still in the parent body regolith, the meteorite was heated to ∼400-600 °C by impacts or solar radiation. Heating led to the amorphisation and dehydroxylation of serpentine, replacement of tochilinite by magnetite, loss of sulphur from the matrix, and modification to the structure of organic matter that includes organic nanoglobules. Significant differences between samples in oxygen isotope compositions, and water/hydroxyl contents, suggests that the meteorite contains lithologies that have undergone different intensities of heating. EET 96029 may be more representative of the true nature of parent body regoliths than many other CM meteorites, and as such can help interpret results from the forthcoming missions to study and return samples from C-complex asteroids.

Genealogy of Iron and Pallasite Meteorites as Revealed by Cr Isotopes

NASA Astrophysics Data System (ADS)

Sanborn, M.; Yin, Q. Z.; Ziegler, K. G.

2017-12-01

The parent bodies and/or chemical reservoirs from which iron and stony-iron meteorites originated are not very well understood. It is unclear if particular groups of iron or stony-iron meteorites originated from melting of already known chondritic parent bodies or are representating new chemical reservoirs. Potential connections between iron meteorites and pallasites and known parent bodies have been suggested based on oxygen isotopes. Proposed genetic relationships include the IVA irons with ordinary chondrites1 and the anomalous pallasite Eagle Station with the CV chondrites2. Here, we use the power of Cr isotopes to further resolve potential connections between IVA irons and pallasites and specific parent bodies. Our new measurements of Cr isotopic composition of silicate inclusions from two IVA irons, Steinbach and São João Nepomuceno, are shown to be indistinguishable from that of the ordinary chondrites. Coupling Cr with oxygen indicates the IVA irons likely originated from the same source as LL chondrites. In contrast with Eagle Station, the new Cr isotope measurements combined with oxygen indicates the MGP Brenham and Krasnojarsk sampled a source material similar to that of the anomalous HEDs. As with Eagle Station, the Milton pallasite exhibits a carbonaceous chondrite (CC) Cr isotope composition, indicating that Eagle Station was not the lone case of a pallasite originating from a CC reservoir. By establishing these genetic relationships using Cr isotopes, it is now evident that the differentiation activity sampled by IVA irons and pallasites represents processes occurring on a diverse set of parent bodies in the early Solar System. [1] Ruzicka and Hutson (2006) MAPS, 41, 1959. [2] Shukolyukov and Lugmair (2006) EPSL, 250, 200.

Geochemistry of Vesta and Ceres: In-flight calibration of Dawn

NASA Astrophysics Data System (ADS)

Prettyman, T. H.; Feldman, W. C.; McSween, H. Y.

2009-04-01

The purpose of the Dawn mission is to investigate processes that contributed to the formation and early evolution of solid bodies in the solar system by exploring Vesta and Ceres, which are the two largest bodies in the main astreroid belt. Because they were formed at different heliocentric distances, Vesta and Ceres incorporated different amounts of water and other volatiles, which strongly influenced their thermal evolution. Vesta, which is thought to be the source of the basaltic, Howardite, Eucrite, and Diogenite (HED) meteorites, is dry and underwent igneous differentiation. In contrast, low-temperature, aqueous processing must have played an important role in the evolution of Ceres, which is rich in water and other volatiles, and may still contain subsurface liquid water. By exploring both Vesta and Ceres, the gradient in the composition of the solar nebula and role of water in planetary evolution can be investigated. The Dawn payload includes redundant framing cameras (FC), a visible and infrared spectrometer (VIR), and a gamma ray and neutron detector (GRaND), which, along with radio science, will measure surface geomorphology, composition, and mineralogy, and provide constraints on the internal structure of Vesta and Ceres. For both Vesta and Ceres, global mapping data will be acquired from circular polar orbits. In low altitude orbits, GRaND will map the elemental composition of Vesta and Ceres to depths less than one meter, including major rock forming elements and light elements (such as H, C, and N), which are the primary constituents of ices. GRaND consists of 21 radiation sensors, which measure the spectrum of neutrons and gamma rays originating from interactions between galactic cosmic rays and the material constituents of the asteroids and, separately, backgrounds from spacecraft materials. GRaND uses a bismuth germanate (BGO) scintillator for gamma ray spectroscopy, which has high efficiency, enabling the measurement of gamma rays up to 10 MeV, including capture gamma rays from Fe and Ti. Below 3 MeV, the BGO sensor works in combination with a 16-element array of CdZnTe semiconductors, which have relatively high resolution, enabling accurate measurement of the densely populated, low energy region of the gamma ray spectrum, which contains gamma rays from radioactive decay (K, Th, and U) and from nuclear reactions (for example, with Mg, Si, and H). Thermal, epithermal, and fast neutrons are measured using a combination of boron-loaded plastic and lithium-loaded glass scintillators. At Vesta, gamma ray and neutron spectroscopy will be used to determine geochemical trends that can be compared with HED data. For example, a scatter plot of the average atomic mass (determined from fast neutrons) and magnesium number can be used to tell the difference between diogenite and eucrite compositions, which are HED end-members. Correlations with MgO (for example, with FeO or SiO2) also strongly differentiate between diogenite and eucrite, and, in combination with optical spectroscopy, can be used to determine whether an olivine-rich mantle is exposed in Vesta's large south polar crater. At Ceres, neutron spectroscopy can be used to determine water abundance and layering (for example, ice may be present in the shallow subsurface at high latitudes), which will provide constraints on recharge and loss mechanisms (for example, emplacement via water volcanism vs. gradual replenishment from a subsurface acquifer). In addition, nuclear spectroscopy can be used to determine the possible presence of CO2 and NH3 ices on the surface of Ceres as well as the composition of non-icy materials, including the hydration state and composition of surface minerals. GRaND was calibrated in the laboratory prior to delivery to the spacecraft. In addition, the response of the instrument to the space radiation environment was measured during Earth-Mars cruise, which followed launch in September of 2007. Because the data were acquired when the energetic particle flux was minimal, the measurements are ideal for determining the background from galactic cosmic rays under conditions that would be ideal for science data acquisition at Vesta and Ceres. In February of 2009, the spacecraft will fly by Mars. At closest approach, the spacecraft will be within 500 km of Mars, providing GRaND with a strong source of planetary neutrons and gamma rays, which will be used to cross-calibrate GRaND against elemental abundance data acquired by the Mars Odyssey Gamma Ray Spectrometer instrument suite. Here, we describe the instrument response model and its application to the analysis of the space radiation background during cruise and cross-calibration against Odyssey data at Mars. The model is applied to determine the expected performance of GRaND at Vesta and Ceres.

Thin-sectioning and analysis of fine-grained meteoritic materials

NASA Technical Reports Server (NTRS)

Brooks, Donald A. (Editor); Bradley, John P.

1992-01-01

The overall theme of the work was the identification of the sources and formation/aggregation mechanisms of the various classes of interplanetary dust particles (IDP's) and to clarify the relationship between IDP's and conventional meteorites. IDP's are believed to be derived from a much broader range of parent bodies than conventional meteorites. Some of these parent bodies (e.g., comets) have escaped that post accretional processing that has affected the parent bodies of meteorites. Therefore, IDP's are likely to preserve a record of early solar system and possibly presolar grain forming reactions. Using analytical electron microscopy (AEM) and more recently micro-infrared (IR) microspectroscopy to examine ultramicrotomed thin sections, we have addressed the questions of IDP formation mechanisms, sources, and their relationship to conventional meteorites. The following sections describe specific findings resulting from these studies.

Lunar and Planetary Science XXXV: Concerning Chondrites

NASA Technical Reports Server (NTRS)

2004-01-01

The Lunar and Planetary Science XXXV session entitled "Concerning Chondrites" includes the following topics: 1) Petrology and Raman Spectroscopy of Shocked Phases in the Gujba CB Chondrite and the Shock History of the CB Parent Body; 2) The Relationship Between CK and CV Chondrites: A Single Parent Body Source? 3) Samples of Asteroid Surface Ponded Deposits in Chondritic Meteorites; 4) Composition and Origin of SiO2-rich Objects in Carbonaceous and Ordinary Chondrites; 5) Re-Os Systematics and HSE distribution in Tieschitz (H3.6); Two Isochrons for One Meteorite; 6) Loss of Chromium from Olivine During the Metamorphism of Chondrites; 7) Very Short Delivery Times of Meteorites After the L-Chondrite Parent Body Break-Up 480 Myr Ago; and 8) The Complex Exposure History of a Very Large L/LL5 Chondrite Shower: Queen Alexandra Range 90201.

Associations between Child Anxiety Symptoms and Child and Family Factors in Pediatric Obesity

PubMed Central

Lim, Crystal S.; Espil, Flint M.; Viana, Andres G.; Janicke, David M.

2015-01-01

Objective The current study compared child weight status, social skills, body dissatisfaction, and health-related quality of life (HRQOL), as well as parent distress and family functioning in youth who are overweight and obese (OV/OB) with versus without clinical anxiety symptoms. Method Participants included 199 children 7–12 years old (Mage= 9.88 years) who were OV/OB and their parents. Children completed social skills, body dissatisfaction, and HRQOL questionnaires. Parents completed the Child Behavior Checklist (CBCL) and child HRQOL, parent distress, family functioning, and demographic questionnaires. Children were placed in two groups based on CBCL Anxiety Problems scale scores; the OV/OB + Clinical Anxiety group included children with T-scores ≥ 65 (n = 23) and children with T-scores ≤ 59 comprised the OV/OB group (n = 176). Results After controlling for covariates, children in the OV/OB + Clinical Anxiety group reported more body dissatisfaction (F [1,198] = 5.26, p =.023, partial η2 = .027) and lower total HRQOL (F [1,198] = 8.12, p = .005, η2=.041) and had parents who reported higher psychological distress (F [1,198] = 5.48, p = .020, η2=.028) and lower child total HRQOL (F [1,198] = 28.23, p < .001, η2=.128) compared to children in the OV/OB group. Group differences were not significant for child weight status, social skills, or family functioning. Conclusion Clinically significant anxiety among children who are OV/OB is associated with increased body dissatisfaction and parent psychological distress, as well as decreased HRQOL. Findings have implications for the assessment and treatment of anxiety symptoms in pediatric obesity. PMID:26468940

Parenting styles and body mass index: a systematic review of prospective studies among children.

PubMed

Sokol, R L; Qin, B; Poti, J M

2017-03-01

Parenting style may be an important determinant of an individual's future weight status. However, reviews that evaluate the relationship between parenting style and weight-related outcomes have not focused on prospective studies. We systematically searched PubMed, Embase and PsychInfo for studies published between 1995 and 2016 that evaluated the prospective relationship between parenting style experienced in childhood and subsequent weight outcomes. We identified 11 prospective cohort studies. Among the eight studies that categorized parenting style into distinct groups (i.e. authoritative, authoritarian, permissive and neglectful), five provided evidence that authoritative parenting was associated with lower body mass index gains. Among the six highest quality studies, four suggested a protective role of authoritative parenting style against adverse weight-related outcomes. However, only one study controlled for a comprehensive set of confounders, and the small number of studies conducted within certain age groups precluded our ability to ascertain critical periods when parenting style is most strongly related to child weight. The present literature supports the idea that authoritative parenting may be protective against later overweight and obesity, although findings are mixed. More prospective cohort studies of longer durations, with more sophisticated methods that examine age-varying relationships, and that control for a comprehensive set of confounders, are needed. © 2017 World Obesity Federation.

Parenting styles and body mass index: A systematic review of prospective studies among children

PubMed Central

Sokol, Rebeccah L; Qin, Bo; Poti, Jennifer M

2017-01-01

Background Parenting style may be an important determinant of an individual's future weight status. However, reviews that evaluate the relationship between parenting style and weight-related outcomes have not focused on prospective studies. Methods We systematically searched PubMed, Embase, and PsychInfo for studies published between 1995-2016 that evaluated the prospective relationship between parenting style experienced in childhood and subsequent weight outcomes. Results We identified eleven prospective cohort studies. Among the eight studies that categorized parenting style into distinct groups (i.e. authoritative, authoritarian, permissive, and neglectful), five provided evidence that authoritative parenting was associated with lower body mass index gains. Among the six highest quality studies, four suggested a protective role of authoritative parenting style against adverse weight-related outcomes. However, only one study controlled for a comprehensive set of confounders, and the small number of studies conducted within certain age groups precluded our ability to ascertain critical periods when parenting style is most strongly related to child weight. Conclusions The present literature supports the idea that authoritative parenting may be protective against later overweight and obesity, although findings are mixed. More prospective cohort studies of longer durations, with more sophisticated methods that examine age-varying relationships, and that control for a comprehensive set of confounders, are needed. PMID:28086262

Teen Development

MedlinePlus

... you might notice include Increased independence from your parents More concerns about body image and clothes More ... problem. If you need help, talk to your parents, school counselor, or health care provider. Centers for ...

Interpretations of family size distributions: The Datura example

NASA Astrophysics Data System (ADS)

Henych, Tomáš; Holsapple, Keith A.

2018-04-01

Young asteroid families are unique sources of information about fragmentation physics and the structure of their parent bodies, since their physical properties have not changed much since their birth. Families have different properties such as age, size, taxonomy, collision severity and others, and understanding the effect of those properties on our observations of the size-frequency distribution (SFD) of family fragments can give us important insights into the hypervelocity collision processes at scales we cannot achieve in our laboratories. Here we take as an example the very young Datura family, with a small 8-km parent body, and compare its size distribution to other families, with both large and small parent bodies, and created by both catastrophic and cratering formation events. We conclude that most likely explanation for the shallower size distribution compared to larger families is a more pronounced observational bias because of its small size. Its size distribution is perfectly normal when its parent body size is taken into account. We also discuss some other possibilities. In addition, we study another common feature: an offset or "bump" in the distribution occurring for a few of the larger elements. We hypothesize that it can be explained by a newly described regime of cratering, "spall cratering", which controls the majority of impact craters on the surface of small asteroids like Datura.

Elephant Moraine 87521 - The first lunar meteorite composed of predominantly mare material

NASA Technical Reports Server (NTRS)

Warren, Paul H.; Kallemeyn, Gregory W.

1989-01-01

This paper presents the results of trace-element analyses and detailed petrography obtained for the Elephant Moraine 87521 meteorite (EET87521) found recently in Antarctica. Its high values found for the Fe/Mn ratio and the bulk-Co content indicate that the EET87521 is not, as was originally classified, a eucrite. Moreover, its low Ga/Al and Na/Ca ratios exclude the possibility that it is an SNC meteorite. These and other characteristics (e.g., a very low Ti content) of the EET87521 suggest its affinity with very-low-Ti high-alumina varieties of lunar mare basalt.

The Meteoritical Bulletin, No. 88, 2004 July

USGS Publications Warehouse

Russell, S.S.; Folco, L.; Grady, M.M.; Zolensky, M.E.; Jones, R.; Righter, K.; Zipfel, J.; Grossman, J.N.

2004-01-01

The Meteoritical Bulletin No. 88 lists information for 1610 newly classified meteorites, comprising 753 from Antarctica, 302 from Africa, 505 from Asia (495 of which are from Oman), 40 from North America, 5 from South America, 4 from Europe, and 1 of unknown origin. Information is provided for 9 falls (Alby sur Che??ran, Al Zarnkh, Devgaon, Kamioka, Kendrapara, Maromandia, New Orleans, Sivas, and Villalbeto de la Pen??a). Noteworthy specimens include a eucrite fall (Alby sur Che??ran), 6 martian meteorites, 13 lunar meteorites, and 12 irons including one weighing 3 metric ions (Dronino). ?? Meteoritical Society, 2004.

Meeting the Challenge of Involving Parents in School. Newsletter

ERIC Educational Resources Information Center

Center for Comprehensive School Reform and Improvement, 2005

2005-01-01

Parent involvement continues to challenge practitioners engaged in school reform despite being a required component of many school improvement initiatives--from Title I Schoolwide Programs to federally mandated school improvement plans. The benefits of parent involvement are clear: A growing body of research shows that successful parent…

A Sexual Learning Curriculum for Parents of Young Children.

ERIC Educational Resources Information Center

Green, Kathryn F.; And Others

The aims of this sexual learning curriculum are to increase parents' emotional and intellectual understanding of human sexuality and to improve their ability to talk about sexuality with their children. Specifically, the curriculum attempts to increase parents' awareness that (1) sexuality includes lifestyle choices, body image, gender role,…

Engaging Parents in Parent Engagement Programs

ERIC Educational Resources Information Center

Levitt, Steven; List, John; Metcalfe, Robert; Sadoff, Sally

2016-01-01

Researchers, policymakers, and educators have long recognized the role of parents in shaping student achievement. A large body of observational studies documents the strong relationship between family background and educational outcomes, but to date there have been very few experimental studies in this area. In this study, the authors offer a…

Teacher-to-Parent Communication: Experimental Evidence from a Low-Cost Communication Policy

ERIC Educational Resources Information Center

Kraft, Matthew A.; Rogers, Todd

2014-01-01

A wide body of literature documents the important role that parents play in supporting children's academic success in school (Houtenville & Conway, 2008; Barnard, 2004; Fan & Chen, 2001). Drawing on this literature, national taskforces and federal legislation consistently identify increased parental involvement as a central goal of…

Ethnic Differences in Parental Attitudes and Beliefs about Being Overweight in Childhood

ERIC Educational Resources Information Center

Trigwell, J.; Watson, P. M.; Murphy, R. C.; Stratton, G.; Cable, N. T.

2014-01-01

Objective: This study examined the relationship between ethnic background and parental views of healthy body size, concerns surrounding overweight and attitudes to perceived causes of overweight in childhood. Method: A self-report questionnaire was designed to explore parental attitudes towards childhood weight. Sampling deliberately…

The Effectiveness of Lifestyle Triple P in the Netherlands: A Randomized Controlled Trial

PubMed Central

Gerards, Sanne M. P. L.; Dagnelie, Pieter C.; Gubbels, Jessica S.; van Buuren, Stef; Hamers, Femke J. M.; Jansen, Maria W. J.; van der Goot, Odilia H. M.; de Vries, Nanne K.; Sanders, Matthew R.; Kremers, Stef P. J.

2015-01-01

Introduction Lifestyle Triple P is a general parenting intervention which focuses on preventing further excessive weight gain in overweight and obese children. The objective of the current study was to assess the effectiveness of the Lifestyle Triple P intervention in the Netherlands. Method We used a parallel randomized controlled design to test the effectiveness of the intervention. In total, 86 child-parent triads (children 4–8 years old, overweight or obese) were recruited and randomly assigned (allocation ratio 1:1) to the Lifestyle Triple P intervention or the control condition. Parents in the intervention condition received a 14-week intervention consisting of ten 90-minute group sessions and four individual telephone sessions. Primary outcome measure was the children’s body composition (BMI z-scores, waist circumference and skinfolds). The research assistant who performed the measurements was blinded for group assignment. Secondary outcome measures were the children’s dietary behavior and physical activity level, parenting practices, parental feeding style, parenting style, and parental self-efficacy. Outcome measures were assessed at baseline and 4 months (short-term) and 12 months (long-term) after baseline. Multilevel multiple regression analyses were conducted to determine the effect of the intervention on primary and secondary outcome measures. Results No intervention effects were found on children’s body composition. Analyses of secondary outcomes showed positive short-term intervention effects on children’s soft-drink consumption and parental responsibility regarding physical activity, encouragement to eat, psychological control, and efficacy and satisfaction with parenting. Longer-term intervention effects were found on parent’s report of children’s time spent on sedentary behavior and playing outside, parental monitoring food intake, and responsibility regarding nutrition. Conclusion Although the Lifestyle Triple P intervention showed positive effects on some parent reported child behaviors and parenting measures, no effects were visible on children’s body composition or objectively measured physical activity. Several adjustments of the intervention content are recommended, for example including a booster session. Trial Registration Nederlands Trial Register NTR 2555 PMID:25849523

Recent disruption of an asteroid from the Eos family

NASA Astrophysics Data System (ADS)

Novaković, B.; Tsirvoulis, G.

2014-07-01

A key difficulty with searching for partially differentiated asteroids arises from the fact that a crust covers the exterior of the body, and, consequently, should hide the melted interior. This motivates an alternative approach of examining members of asteroid families, i.e., fragments of single large bodies, many of which were in the size regime capable of igneous differentiation, that have been disrupted by catastrophic collisions. Such families could provide a stratigraphic cross section across the interior of the parent asteroid [1]. With more than 10,000 known members, the Eos dynamical family is one of the most numerous and earliest recognized asteroid families [2]. Interestingly, the estimated ˜220-km-diameter parent body [3] is well within the size range capable of differentiation. Thus, existing family members should contain fragments of the deep interior. The Eos family has the highest diversity of taxonomic classes than any other known family [4]. Many members are of K spectral type, which is uncommon outside the family, and is similar to the spectra of CV, CK, CO, and CR carbonaceous chondrites [5]. This diversity leads to the suggestion that the Eos parent body was partially differentiated [4,6]. Thus, the Eos family may not only be a remnant of a partially differentiated parent body, but it could be the source of the CV-CK meteorite group. Here we report the discovery of a young subfamily of the Eos asteroid family. It may help understanding the mineralogical nature of the Eos asteroid family and of its parent body. By applying the hierarchical clustering method [7], we find an extremely compact 16-body cluster within the borders of the Eos family. We name the cluster (6733) 1992 EF, after its largest member. The statistical significance of this new cluster is estimated to be above 99%, indicating that its members share a common origin. All members of the cluster are found to be dynamically stable over long timescales. Backward numerical orbital integrations are used to set an upper limit of the age of the cluster to be only 4 Myr.

Parental bonds and body dissatisfaction in a clinical sample: The mediating roles of attachment anxiety and media internalization.

PubMed

Grenon, Renee; Tasca, Giorgio A; Maxwell, Hilary; Balfour, Louise; Proulx, Genevieve; Bissada, Hany

2016-12-01

We evaluated an attachment theory model in which mother and father care were hypothesized to be indirectly related to body dissatisfaction mediated by attachment anxiety and media internalization. Participants were 232 women diagnosed with an eating disorder who completed a retrospective measure of parental bonds, and measures of attachment anxiety, media internalization, and body image. Mother care was negatively associated with body dissatisfaction, suggesting that recollection of mothers as less caring was directly related to poorer body image. Lower father care, was indirectly associated with greater body dissatisfaction mediated by higher attachment anxiety and higher media internalization. That is, women with an eating disorder who recollected fathers as less caring had higher attachment anxiety, which was related to greater internalizing of media-related thin ideals, that in turn was associated with poorer body image. Mothers and fathers may impact body dissatisfaction by differing mechanisms in clinical samples. Copyright © 2016 Elsevier Ltd. All rights reserved.

Association of lifestyle and body structure to ocular axial length in Japanese elementary school children.

PubMed

Terasaki, Hiroto; Yamashita, Takehiro; Yoshihara, Naoya; Kii, Yuya; Sakamoto, Taiji

2017-07-12

The purpose of this study is to determine whether the lifestyle and body stature are significantly associated with the axial length (AL) of the eyes of Japanese third grade students. A prospective, cross sectional, observational study was performed on 122 third grade students consisting of 61 boys and 61 girls ages 8 to 9 years. The AL, body height, body weight, and body mass index (BMI) were measured. The lifestyle was determined by activities such as the daily duration of indoor studying, television viewing, use of computers and smart phones, outdoor activity time, bed time, Japanese or Western dietary habits, and parental myopia were investigated by a questionnaire with three or five grade levels. The relationship between AL and the questionnaire variables were analyzed by Spearman's correlation analyses. Westernized dietary habits (r = -0.24, P = 0.01), duration of computer and smart phone use (r = 0.24, P = 0.008), parental myopia (r = 0.39, P < 0.001), body weight (r = 0.26, P = 0.005), and BMI (r = 0.23, P = 0.011) were significantly correlated with the AL. Multiple logistic regression analyses showed that the sex [r = -0.48; 95% confidence interval (CI) -0.80 to -0.17, P = 0.003], body weight (r = 0.04; 95% CI 0.02 to 0.07, P = 0.038), westernized dietary habits (r = -0.30; 95% CI -0.55 to -0.05, P = 0.021), and parental myopia (r = 0.40; 95% CI 0.20 to 0.61, P < 0.001) were significantly and independently correlated with the AL. The body weight and parental myopia and westernized dietary habits are factors significantly associated with myopia. Changing from Japanese food style to westernized food style might increase the risk of progression of school myopia.

Gender and Body-Fat Status as Predictors of Parental Feeding Styles and Children's Nutritional Knowledge, Eating Habits and Behaviours.

PubMed

Lipowska, Małgorzata; Lipowski, Mariusz; Jurek, Paweł; Jankowska, Anna M; Pawlicka, Paulina

2018-04-25

The home food environment is critically important for the development of children’s health-related practices. By managing dietary restrictions, providing nutritional knowledge and demonstrating eating behaviours, parents contribute to children’s food preferences and eating patterns. The present study examined nutritional knowledge, eating habits and appetite traits among 387 Polish five-year-old healthy and overfat boys and girls in the context of parental feeding styles and body-fat status. We observed that girls presented healthier eating habits than boys; however, overfat boys had better nutritional knowledge. Children’s body-fat percentage (%BF) was found to be linked with eating behaviours such as low satiety responsiveness and increased food responsiveness in girls as well as low emotional undereating and increased emotional overeating in boys. Our results revealed that overfat mothers, who were more prone to use the encouragement feeding style, rarely had daughters with increased %BF. Parents of overfat girls, however, were less likely to apply encouragement and instrumental feeding styles. Contrary to popular belief and previous studies, overfat women do not necessarily transmit unhealthy eating patterns to their children. Parents’ greater emphasis on managing the weight and eating habits of daughters (rather than sons) probably results from their awareness of standards of female physical attractiveness.

Risk factors for otolaryngological foreign bodies in Eastern Poland.

PubMed

Rybojad, Beata; Niedzielski, Artur; Niedzielska, Grazyna; Rybojad, Pawel

2012-11-01

To identify the sociodemographic characteristics and risk factors associated with suspected foreign bodies in the ear, nose, throat, airway, and esophagus among Polish children. Case series with chart review. Setting Tertiary care medical center. A retrospective analysis of the medical records of patients hospitalized for a suspected foreign body (FB) between 1998 and 2008 was conducted. Data regarding place of residence, presence of siblings, parents' educational status, seasonality, psychomotor development, age, and sex were collected and statistically analyzed. Of the 1011 patients with suspected foreign body insertion, 849 (84%) had a positive diagnosis. Of the confirmed foreign bodies, 96 were found in the tracheobronchial tree, 142 were found in the esophagus, and 611 were located in the external auditory canals, nasopharyngeal passage, tonsils, auricles, or lips. Sociodemographically, 596 of the children came from urban areas, with a preponderance of males (55%). Objects were removed more frequently in summer and autumn (60%). Children with siblings (53%) predominated. The majority of patients (52%) had parents with an elementary education. Food was the most frequent foreign body in children under 3 years of age. Patients with delayed psychomotor development constituted 1.6% of the analyzed population. Being male, 1 to 3 years of age, belonging to an urban family with siblings, and having parents with an elementary education increased the risk of foreign body insertion. Training caregivers about proper nutrition and safety rules when playing with children can reduce the risk of accidents related to foreign body insertion.

A Thermal Model for the Differentiation of Asteroid 4 Vesta, Based on Radiogenic and Collisional Heating

NASA Astrophysics Data System (ADS)

Ghosh, Amitabha

A finite element code has been developed to study the thermal history of asteroid 4 Vesta. This is the first attempt to model the thermal history of a differentiated asteroid, from accretion through core and crust formation and subsequent cooling until geochemical closure is attained. Previous thermal models were simpler formulations aimed at explaining metamorphism and aqueous alteration in unmelted asteroids. The results of the simulation are consistent with chronological measurements of cumulate and noncumulate eucrites, meteorites belonging to the HED suite, believed to have been derived from 4 Vesta. The work solves major problems with the hypothesis of heating by decay of 26Al, an extinct radionuclide, believed to be a plausible heat source in the early solar system. The simulation draws a model chronology of Vesta and predicts the time interval of accretion at 2.85 Myrs, the absolute times (with respect to CAI formation) of core formation at 4.58 Myrs, crust formation at 6.58 Myrs and geochemical closure on Vesta at ~100 Myrs. It is concluded that neither collisional heating nor heating due to the radioactive decay of 60Fe caused any perceptible difference in the whole-body thermal history of Vesta. Further, the thermal model suggested that the olivine-rich spot observed on Vesta may not be excavated mantle material, but may be unmelted near-surface material that escaped the asteroid's differentiation history.

Parents of elementary school students weigh in on height, weight, and body mass index screening at school.

PubMed

Kubik, Martha Y; Fulkerson, Jayne A; Story, Mary; Rieland, Gayle

2006-12-01

School-based body mass index (BMI) screening and parent notification programs have been recommended as a childhood overweight prevention strategy. However, there are little empirical data available to guide decision making about the acceptability and safety of programs. A pilot study was conducted using a quasiexperimental research design. In fall 2004, children in 4 suburban elementary schools (kindergarten to sixth grade) in the St Paul/Minneapolis, MN, metropolitan area completed height/weight screening. The following spring, parents in 2 schools received letters containing height/weight and BMI results. A self-administered post-only survey examined parents' opinions and beliefs regarding school-based BMI screening and parent notification programs (response rate: 790/1133 = 70%). The chi2 test of significance was used to examine differences in program support by treatment condition, child's weight status, and sociodemographic characteristics. Among all parents, 78% believed it was important for schools to assess student's height/weight annually and wanted to receive height, weight, and BMI information yearly. Among parents receiving the letter, 95% read most/all of the letter. Most parents (80%) and children (83%) reported comfort with the information in the letter. Parents of overweight children were more likely to report parental discomfort as well as child discomfort with letter content. There was considerable parental support for school-based BMI screening and parent notification programs. Programs may be a useful overweight prevention tool for children. However, continued attention to how best to support parents and children affected by overweight is required.

Sociocultural pressures and adolescent eating in the absence of hunger

PubMed Central

Reina, Samantha A.; Shomaker, Lauren B.; Mooreville, Mira; Courville, Amber B.; Brady, Sheila M.; Olsen, Cara; Yanovski, Susan Z.; Tanofsky-Kraff, Marian; Yanovski, Jack A.

2013-01-01

Parental feeding practices and sociocultural pressures theoretically influence eating behavior. Yet, whether these factors relate to eating in the absence of hunger (EAH) is unknown. We assessed if sociocultural pressures were associated with EAH among 90 adolescents (Mage = 15.27, SD = 1.39; 48% female). Parents completed the Child Feeding Questionnaire. Adolescents completed the Perceived Sociocultural Pressures Scale, Sociocultural Attitudes Towards Appearance Questionnaire-3, and Multidimensional Body Self-Relations Questionnaire-Appearance Scales. On two occasions, EAH was assessed as snack food intake after adolescents ate to satiety. Controlling for body composition and demographics, parental restriction and family pressure to be thin were associated with greater EAH. Media pressure was related to more EAH in girls. Appearance orientation and preoccupation with becoming overweight mediated links between sociocultural pressures and EAH. Findings support the notion that sociocultural pressures and their links to body image may contribute to the course of disinhibited eating behaviors during adolescence. PMID:23394966

Chondritic Meteorites: Nebular and Parent-Body Formation Process

NASA Technical Reports Server (NTRS)

Rubin, Alan E.

1997-01-01

Chondritic meteorites are the products of condensation, agglomeration and accretion of material in the solar nebula; these objects are the best sources of information regarding processes occurring during the early history of the solar system. We obtain large amounts of high-quality chemical and petrographic data and use them to infer chemical fractionation processes that occurred in the solar nebula and on meteorite parent bodies during thermal metamorphism, shock metamorphism and aqueous alteration. We compare diverse groups of chondrites and model their different properties in terms of processes that differed at different nebular locations or on different parent-bodies. In order to expand our set of geochemically important elements (particularly Si, C, P and S) and to distinguish the different oxidation states of Fe, Greg Kallemeyn spent three months (1 Sept. - 30 Nov. 1995) at the Smithsonian Institution to learn Eugene Jarosewich's wet chemical techniques. Key specimens from the recently established CK, CR and R chondrite groups were analyzed.

Is children's Body Mass Index associated with their parents' personality? A prospective controlled trial.

PubMed

Erdoğan, Fırat; Eliaçik, Mustafa; Özahi Ipek, İlke; Arici, Neslihan; Kadak, Muhammed T; Ceran, Ömer

2017-08-01

The aim of this study was to elucidate the effect of the personal characteristics and psychological status of parents on their children's Body Mass Index (BMI) by using validated questionnaires. Obese and healthy control group was assessed with The Parental Attitude Research Instrument (PARI) for the evaluation of parental attitudes towards their children. Additionally, Depression Anxiety and Stress Scale (DASS) were used to assess the relationships between parental depression, anxiety, stress and childhood obesity. A total of 105 children and their parents were divided into two groups. The study group consisted of 58 children with a BMI of higher than 85th percentile whereas 47 children with normal BMI (<85th percentile) were included as the control group. In both groups, the BMI of mothers which is between 25-and 30 kg/m2 and >30 kg/m2 had significant impact on the risk of children's obesity status 1.12-fold and 3.68-fold respectively. The PARI results provided that the children who had disciplined, over-protective parents and those in the parental incompatibility group had higher risk of being obese. Analysis of the DASS Test results showed that children having depressed parents had significantly higher risk of obesity than children whose parents were not depressed (P<0.05). Our results provided that, the parent's status such as obesity, depression and strict personal behaviors have negative impact on their children's weight which is resulting with obesity.

Parenting styles and body mass index trajectories from adolescence to adulthood.

PubMed

Fuemmeler, Bernard F; Yang, Chongming; Costanzo, Phil; Hoyle, Rick H; Siegler, Ilene C; Williams, Redford B; Ostbye, Truls

2012-07-01

Parenting styles such as authoritarian, disengaged, or permissive are thought to be associated with greater adolescent obesity risk than an authoritative style. This study assessed the relationship between parenting styles and changes in body mass index (BMI) from adolescence to young adulthood. The study included self-reported data from adolescents in the National Longitudinal Study of Adolescent Health. Factor mixture modeling, a data-driven approach, was used to classify participants into parenting style groups based on measures of acceptance and control. Latent growth modeling (LGM) identified patterns of developmental changes in BMI. After a number of potential confounders were controlled for, parenting style variables were entered as predictors of BMI trajectories. Analyses were also conducted for male and female individuals of 3 racial-ethnic groups (Hispanic, black, white) to assess whether parenting styles were differentially associated with BMI trajectories in these 6 groups. Parenting styles were classified into 4 groups: authoritarian, disengaged, permissive, and balanced. Compared with the balanced parenting style, authoritarian and disengaged parenting styles were associated with a less steep average BMI increase (linear slope) over time, but also less leveling off (quadratic) of BMI over time. Differences in BMI trajectories were observed for various genders and races, but the differences did not reach statistical significance. Adolescents who reported having parents with authoritarian or disengaged parenting styles had greater increases in BMI as they transitioned to young adulthood despite having a lower BMI trajectory through adolescence.

Parenting Styles and Body Mass Index Trajectories From Adolescence to Adulthood

PubMed Central

Fuemmeler, Bernard F.; Yang, Chongming; Costanzo, Phil; Hoyle, Rick H.; Ph.D.; Siegler, Ilene C.; Williams, Redford B.; Østbye, Truls

2013-01-01

Objective Parenting styles such as authoritarian, disengaged, or permissive are thought to be associated with greater adolescent obesity risk than an authoritative style. This study assessed the relationship between parenting styles and changes in body mass index (BMI) from adolescence to young adulthood. Methods The study included self-reported data from adolescents in the National Longitudinal Study of Adolescent Health. Factor mixture modeling, a data-driven approach, was used to classify participants into parenting style groups based on measures of acceptance and control. Latent growth modeling (LGM) identified patterns of developmental changes in BMI. After a number of potential cofounders were controlled for, parenting style variables were entered as predictors of BMI trajectories. Analyses were also conducted for males and females of three racial/ethnic groups (Hispanic, black, white) to assess whether parenting styles were differentially associated with BMI trajectories in these 6 groups. Results Parenting styles were classified into 4 groups: authoritarian, disengaged, permissive, and balanced. Compared with the balanced parenting style, authoritarian and disengaged parenting styles were associated with a less steep average BMI increase (linear slope) over time, but also less leveling off (quadratic) of BMI over time. Differences in BMI trajectories were observed for various genders and races, but the differences did not reach statistical significance. Conclusions Adolescents who reported having parents with authoritarian or disengaged parenting styles had greater increases in BMI as they transitioned to young adulthood despite having a lower BMI trajectory through adolescence. PMID:22545979

Can the Internet be used to reach parents for family-based childhood obesity interventions?

PubMed

Hohman, Katherine H; Price, Sarah N; Sonneville, Kendrin; Rifas-Shiman, Sheryl L; Gortmaker, Steven L; Gillman, Matthew W; Taveras, Elsie M

2012-04-01

This study aimed to identify socioeconomic correlates of computer/Internet use among parents of overweight preschool-aged children. A total of 470 baseline participants in a trial to prevent obesity in children 2 to 6.9 years old with body mass index ≥ 95th percentile or 85th to 95th percentile with one overweight parent were studied. Interviews with parents used Health Information National Trends Survey questions. Overall, 94% of the participants had home computers and 93% reported Internet usage. In adjusted models, parents with ≤ college degree (odds ratio = 4.8; 95% confidence interval = 1.2-18.3) or with household income ≤$50,000 (odds ratio = 7.6; 95% confidence interval = 2.2-26.8) had decreased likelihood of computer ownership. Of parents who reported going online, 63% used Internet to look for health/medical information for themselves and 42% for their children. Parents with ≤ a college degree or with body mass index <25 kg/m(2) were less likely to use Internet. Results support using the Internet for early childhood obesity prevention with enhanced outreach efforts for low socioeconomic status families.

Socioeconomic Status and Body Mass Index Among Hispanic Children of Immigrants and Children of Natives

PubMed Central

Van Hook, Jennifer

2009-01-01

Objectives. We examined how Hispanic parents' income and education, combined with their nativity status, influenced the body mass index (BMI) of their children, compared with non-Hispanic White children and their parents. Methods. We used data from the Early Childhood Longitudinal Study, Kindergarten Class of 1998–99 to estimate linear growth curve models of children's initial BMI in kindergarten and change in BMI through fifth grade. Socioeconomic status was measured by logged household income and parental educational attainment (less than high school, high school graduate, some college, college graduate or higher). Results. Parental education was negatively associated with children's BMI (baseline and growth) for non-Hispanic White children. Among Hispanic children, the association of parental education with growth in BMI was negative but much weaker. The weak effect of parental education was not explained by the presence of immigrants in the Hispanic population. Income was strongly negatively associated with children's BMI in kindergarten among children of Hispanic and White natives, but positively associated among Hispanic immigrant families. Conclusions. The positive income–BMI association among Hispanic immigrant children might reflect cultural differences that immigrant parents carry with them from their countries of origin. PMID:19846690

Parental Perceptions of Body Mass Index Notification: A Qualitative Study.

PubMed

Schwartz, Misty

2015-10-01

There is a worldwide epidemic of obesity in children. To address obesity in children, emphasis must be on factors within family, school, and community environments. Although most parents and school officials are aware of the problem of overweight children, there are few data available to guide decision making about the acceptability of school-based body mass index (BMI) screening and referral programs. Parental insight is essential to determine the efficiency and effectiveness of BMI notification. The purpose of this qualitative study was to explore the perceptions of parents whose school-age children received a BMI referral letter stating their child is overweight. Purposeful convenience sampling was used to obtain 21 parents. Semistructured interviews were used to collect the data. Eight themes and corresponding subthemes emerged. The themes regarding parental perceptions were feelings about receiving the letter, causes of obesity, capabilities, barriers, role modeling, primary care provider response, school's role, and health screening process. The findings of this study can serve as the foundation and provide guidance for parents, schools, healthcare professionals, and communities when attempting to implement changes and programs to combat the epidemic of childhood obesity. © 2015, American School Health Association.

Parents' Experiences with Services and Treatment for Their Children Diagnosed with Cerebral Palsy

ERIC Educational Resources Information Center

Knis-Matthews, Laurie; Falzarano, Mary; Baum, Deborah; Manganiello, Jennifer; Patel, Sargam; Winters, Laura

2011-01-01

While there is a considerable body of knowledge investigating the efficacy of constraint-induced movement therapy (CIMT), there is a need for information focusing on parents' experiences when their children receive these services. This qualitative research study initially explored the experiences of four parents with children who are diagnosed…

Parental Perceptions of the Rural School's Role in Addressing Childhood Obesity

ERIC Educational Resources Information Center

Stalter, Ann M.; Kaylor, Marybeth; Steinke, Jessica D.; Barker, Rosanta M.

2011-01-01

This study employed cross-sectional, descriptive design with convenience sampling to explore rural parent perceptions of child obesity, use of Body Mass Index (BMI) in schools, preferences for receipt of BMI information and, the rural school's role in obesity prevention/treatment. The survey "Parental Perceptions of BMI and Obesity in the…

Motivations of Parental Involvement in Children's Learning: Voices from Urban African American Families of Preschoolers

ERIC Educational Resources Information Center

Huang, Grace Hui-Chen; Mason, Kimberly L.

2008-01-01

A growing body of research supports the view that parents' attitudes, behaviors, and activities related to children's education influences students' learning and educational success. To date, research studying parental involvement in their children's schooling included elementary through middle school aged populations. There have been a few…

Parental perception and child's nutritional status.

PubMed

Yalçın, S Songül; Serdaroğlu, Esra; İnce, O Tolga

2016-01-01

Childhood obesity is a health hazard increasing worldwide. Preschool period which is under supervision of parents is a critical period to detect overweight and take precautions. We studied the factors affecting parental estimation of their preschool child's weight. Three hundred sixty seven mothers completed questionnaires consisting of child's and parents' anthropometric measurements, parents' assessment of their child's and their own weight status, and general information about their lifestyle. Mothers also chose their wish for current and future body image of their child from child drawings representing percentiles. Child body mass index-for-age z score (BAZ) was related to birth weight and child's appetite. BAZ was not related to child's gender, presence of chronic disease, family pattern, parental age, education or income. 43.1 % of mothers correctly assessed child's BAZ verbally. Maternal verbal estimation was correlated with maternal visual estimation, paternal verbal estimation and child's BAZ. Mothers' wish for future figure of the child was not related to child's BAZ, but showed correlation with mothers' wish for current figure of the child. Mother's correct perception of her child's weight was found to be high, consistent with her spouse and related to child's BAZ.

Exploring Vaccine Hesitancy Through an Artist-Scientist Collaboration : Visualizing Vaccine-Critical Parents' Health Beliefs.

PubMed

Koski, Kaisu; Holst, Johan

2017-09-01

This project explores vaccine hesitancy through an artist-scientist collaboration. It aims to create better understanding of vaccine hesitant parents' health beliefs and how these influence their vaccine-critical decisions. The project interviews vaccine-hesitant parents in the Netherlands and Finland and develops experimental visual-narrative means to analyse the interview data. Vaccine-hesitant parents' health beliefs are, in this study, expressed through stories, and they are paralleled with so-called illness narratives. The study explores the following four main health beliefs originating from the parents' interviews: (1) perceived benefits of illness, (2) belief in the body's intelligence and self-healing capacity, (3) beliefs about the "inside-outside" flow of substances in the body, and (4) view of death as a natural part of life. These beliefs are interpreted through arts-based diagrammatic representations. These diagrams, merging multiple aspects of the parents' narratives, are subsequently used in a collaborative meaning-making dialogue between the artist and the scientist. The resulting dialogue contrasts the health beliefs behind vaccine hesitancy with scientific knowledge, as well as the authors' personal, and differing, attitudes toward these.

Parental perceptions of weight terminology that providers use with youth.

PubMed

Puhl, Rebecca M; Peterson, Jamie Lee; Luedicke, Joerg

2011-10-01

Little research has been performed to examine patient perceptions of weight-related language, especially related to childhood obesity. In this study we assessed parental perceptions of weight-based terminology used by health care providers to describe a child's excess weight and assessed perceived connotations associated with these terms including stigma, blame, and motivation to reduce weight. A national sample of American parents with children aged 2 to 18 years (N = 445) completed an online survey to assess their perceptions of 10 common terms to describe excess body weight in youth (including "extremely obese," "high BMI," "weight problem," "unhealthy weight," "weight," "heavy," "obese," "overweight," "chubby," and "fat"). Parents were asked to use a 5-point rating scale to indicate how much they perceived each term to be desirable, stigmatizing, blaming, or motivating to lose weight. Regression models revealed that the terms "weight" and "unhealthy weight" were rated as most desirable, and "unhealthy weight" and "weight problem" were rated as the most motivating to lose weight. The terms "fat," "obese," and "extremely obese" were rated as the most undesirable, stigmatizing, blaming, and least motivating. Parents' ratings were consistent across sociodemographic variables, body weight, and child's body weight. The results of this study have important implications for the improvement of health care for youth with obesity; it may be advantageous for health care providers to use or avoid using specific weight-based language during discussions about body weight with families. Pediatricians play a key role in obesity prevention and treatment, but their efforts may be undermined by stigmatizing or offensive language that can hinder important discussions about children's health.

Familial Risk of Chronic Musculoskeletal Pain and the Importance of Physical Activity and Body Mass Index: Prospective Data from the HUNT Study, Norway.

PubMed

Lier, Ragnhild; Mork, Paul Jarle; Holtermann, Andreas; Nilsen, Tom Ivar Lund

2016-01-01

The main objectives of the current study was i) to prospectively examine if chronic musculoskeletal pain in parents is associated with risk of chronic musculoskeletal pain in their adult offspring, and ii) to assess if these parent-offspring associations are modified by offspring body mass index and leisure time physical activity. We used data on 4,742 adult offspring linked with their parents who participated in the population-based HUNT Study in Norway in 1995-97 and in 2006-08. Family relations were established through the national Family Registry. A Poisson regression model was used to estimate relative risk (RR) with 95% confidence interval (CI). In total, 1,674 offspring (35.3%) developed chronic musculoskeletal pain during the follow-up period of approximately 11 years. Both maternal (RR: 1.26, 95% CI: 1.03, 1.55) and paternal chronic musculoskeletal pain (RR: 1.29, 95% CI: 1.06, 1.57) was associated with increased risk of offspring chronic musculoskeletal pain. Compared to offspring of parents without chronic musculoskeletal pain, the adverse effect of parental pain was somewhat stronger among offspring who reported a low (RR: 1.82, 95% CI: 1.32, 2.52) versus high (RR: 1.32, 95% CI: 0.95, 1.84) level of leisure time physical activity. Offspring of parents with chronic musculoskeletal pain and who were classified as obese had more than twofold increased risk (RR: 2.33, 95% CI: 1.68, 3.24) of chronic musculoskeletal pain compared to normal weight offspring of parents without pain. In conclusion, parental chronic musculoskeletal pain is positively associated with risk of chronic musculoskeletal pain in their adult offspring. Maintenance of normal body weight may reduce the risk of chronic musculoskeletal pain in offspring of pain-afflicted parents.

Familial Risk of Chronic Musculoskeletal Pain and the Importance of Physical Activity and Body Mass Index: Prospective Data from the HUNT Study, Norway

PubMed Central

Lier, Ragnhild; Mork, Paul Jarle; Holtermann, Andreas; Nilsen, Tom Ivar Lund

2016-01-01

The main objectives of the current study was i) to prospectively examine if chronic musculoskeletal pain in parents is associated with risk of chronic musculoskeletal pain in their adult offspring, and ii) to assess if these parent-offspring associations are modified by offspring body mass index and leisure time physical activity. We used data on 4,742 adult offspring linked with their parents who participated in the population-based HUNT Study in Norway in 1995–97 and in 2006–08. Family relations were established through the national Family Registry. A Poisson regression model was used to estimate relative risk (RR) with 95% confidence interval (CI). In total, 1,674 offspring (35.3%) developed chronic musculoskeletal pain during the follow-up period of approximately 11 years. Both maternal (RR: 1.26, 95% CI: 1.03, 1.55) and paternal chronic musculoskeletal pain (RR: 1.29, 95% CI: 1.06, 1.57) was associated with increased risk of offspring chronic musculoskeletal pain. Compared to offspring of parents without chronic musculoskeletal pain, the adverse effect of parental pain was somewhat stronger among offspring who reported a low (RR: 1.82, 95% CI: 1.32, 2.52) versus high (RR: 1.32, 95% CI: 0.95, 1.84) level of leisure time physical activity. Offspring of parents with chronic musculoskeletal pain and who were classified as obese had more than twofold increased risk (RR: 2.33, 95% CI: 1.68, 3.24) of chronic musculoskeletal pain compared to normal weight offspring of parents without pain. In conclusion, parental chronic musculoskeletal pain is positively associated with risk of chronic musculoskeletal pain in their adult offspring. Maintenance of normal body weight may reduce the risk of chronic musculoskeletal pain in offspring of pain-afflicted parents. PMID:27082110

Lifestyle Triple P: a parenting intervention for childhood obesity.

PubMed

Gerards, Sanne M P L; Dagnelie, Pieter C; Jansen, Maria W J; van der Goot, Lidy O H M; de Vries, Nanne K; Sanders, Matthew R; Kremers, Stef P J

2012-04-03

Reversing the obesity epidemic requires the development and evaluation of childhood obesity intervention programs. Lifestyle Triple P is a parent-focused group program that addresses three topics: nutrition, physical activity, and positive parenting. Australian research has established the efficacy of Lifestyle Triple P, which aims to prevent excessive weight gain in overweight and obese children. The aim of the current randomized controlled trial is to assess the effectiveness of the Lifestyle Triple P intervention when applied to Dutch parents of overweight and obese children aged 4-8 years. This effectiveness study is called GO4fit. Parents of overweight and obese children are being randomized to either the intervention or the control group. Those assigned to the intervention condition receive the 14-week Lifestyle Triple P intervention, in which they learn a range of nutritional, physical activity and positive parenting strategies. Parents in the control group receive two brochures, web-based tailored advice, and suggestions for exercises to increase active playing at home. Measurements are taken at baseline, directly after the intervention, and at one year follow-up. Primary outcome measure is the children's body composition, operationalized as BMI z-score, waist circumference, and fat mass (biceps and triceps skinfolds). Secondary outcome measures are children's dietary behavior and physical activity level, parenting practices, parental feeding style, parenting style, parental self-efficacy, and body composition of family members (parents and siblings). Our intervention is characterized by a focus on changing general parenting styles, in addition to focusing on changing specific parenting practices, as obesity interventions typically do. Strengths of the current study are the randomized design, the long-term follow-up, and the broad range of both self-reported and objectively measured outcomes. Current Controlled Trials NTR 2555 MEC AZM/UM: NL 31988.068.10 / MEC 10-3-052.

Mineralogical Composition of the Different Types of Bright Deposits on Vesta

NASA Technical Reports Server (NTRS)

Zambon, F.; Capaccioni, F.; DeSanctis, M. C.; Ammannito, E.; Li, J.-Y.; Longobardo, A.; Mittlefehldt, D. W.; Palomba, E.; Pieters, C. M.; Schroeder, S. E.;

Neutron Absorption Measurements Constrain Eucrite-Diogenite Mixing in Vesta's Regolith

NASA Technical Reports Server (NTRS)

Prettyman, T. H.; Mittlefehldt, D. W.; Feldman, W. C.; Hendricks, J. S.; Lawrence, D. J.; Peplowski, P. N.; Toplis, M. J.; Yamashita, N.; Beck, A.; LeCorre, L.;

Brief report: parenting styles and obesity in Mexican American children: a longitudinal study.

PubMed

Olvera, Norma; Power, Thomas G

2010-04-01

To assess longitudinally the relations between four parenting styles (authoritative, authoritarian, uninvolved, and indulgent) and child weight status in Mexican American families. Sixty-nine low-income Mexican American mothers and their 4- to 8-year-old children participated in a 4-year longitudinal study. Mothers completed demographic and parenting measures. Children's body weight and height were assessed annually. Body mass index was calculated to determine weight status. At baseline, 65% of children were found to be normal weight, 14% were overweight, and 21% were obese. Analyses examined how parenting styles at baseline predicted child's weight status 3 years later, controlling for initial weight status. Children of indulgent mothers were more likely to become overweight 3 years later than children of authoritative or authoritarian mothers. This study provides longitudinal evidence for the role of indulgent parenting in predicting overweight in Mexican American children. Possible mediating factors that may account for this relationship (e.g., dietary patterns, physical activity patterns, and children's self-regulation) are considered.

Positive parenting mitigates the effects of poor self-regulation on body mass index trajectories from ages 4-15 years.

PubMed

Connell, Lauren E; Francis, Lori A

2014-08-01

This study sought to determine whether parenting style moderates the effects of delay of gratification on body mass index (BMI) trajectories from ages 4-15 years. Longitudinal data were analyzed for 778 children drawn from the Study of Early Child Care and Youth Development. Parenting style (i.e., authoritative, authoritarian, permissive, and neglectful) was created from measures of mothers' sensitivity and expectations for self-control when children were age 4 years. Self-regulation was also measured at 4 years using a well-known delay of gratification protocol. BMI was calculated from measured height and weight at each time point. Mixed modeling was used to test the interaction of parenting styles and ability to delay gratification on BMI trajectories from 4-15 years. There was a significant interaction effect of parenting and ability to delay on BMI growth from 4-15 years for boys. Boys who had authoritarian mothers and failed to delay gratification had a significantly steeper rate of growth in BMI from childhood through adolescence than children in any other parenting by delay group. Authoritative and permissive parenting styles were protective against more rapid BMI gains for boys who could not delay gratification. Ability to delay gratification was protective against BMI gains for boys who had parents with authoritarian or neglectful parenting styles.

Observed and perceived parental overprotection in relation to psychosocial adjustment in preadolescents with a physical disability: the mediational role of behavioral autonomy.

PubMed

Holmbeck, Grayson N; Johnson, Sharon Z; Wills, Karen E; McKernon, Wendy; Rose, Brigid; Erklin, Shannon; Kemper, Therese

2002-02-01

The purpose of this study was to tes a mediational model of associations between parental overprotectiveness (OP), behavioral autonomy. and psychosocial adjustment in 68 families with 8- and 9-year-old preadolescents with spipa bifida and a demographically matched sample of 68 families with able-bodied children. Measures included questionnaire and observational assessments of parental OP; parent and child reports of behavioral autonomy; and parent, child, and teacher reports of preadolescent adjustment. On the basis of both questionnaire and observational measures of OP, mothers and fathers of children with spina bifida were significantly more overprotective than their counterparts in the able-bodied sample, although this group difference was partially mediated by children's cognitive ability. Across samples, mothers were more likely to be overprotective than fathers. Both questionnaire and observational measures of parental OP were associated with lower levels of preadolescent decision-making autonomy as well as with parents being less willing to grant autonomy to their offspring in the future. For the questionnaire measure of OP, and only for the spina bifida sample. the mediational model was supported such that parental OP was associated with less behavioral autonomy, which was, in turn, associated with more externalizing problems. Findings are discussed in relation to the literature on parenting, autonomy development, and pediatric psychology.

Alteration and formation of rims on the CM parent body

NASA Technical Reports Server (NTRS)

Browning, Lauren B.; Mcsween, Harry Y., Jr.; Zolensky, Michael

1994-01-01

All types of coarse-grained components in CM chondrites are surrounded by fine-grained dust coatings, but the origin of these rims is not yet clear. Although a strictly nebular origin seems likely for rims in the relatively unaltered type 3 chondrites, the rims in CM chondrites are dominated by secondary alteration phases. It has been argued that either the coarse-grained cores accreted altered rim materials while still in the nebula or that alteration of primary rim phases occurred on the CM parent body. To constrain the origin of alteration phases in rim material, we have analyzed the textures and mineral associations from 10 CM chondritic falls by optical and scanning electron microscopy. Our results indicate that the secondary phases in CM chondritic rims were produced by parent body fluid-rock interactions which redefined some primary rim textures and may have produced, in some cases, both coarse-grained components and the rims that surround them. Textural features demonstrate the interactive exchange of alteration fluids between rims, matrix, and chondrules on the CM parent body. For example, most matrix-rim contacts are gradational, suggesting the synchronous alteration of both components. Several observations suggest the possibility of in situ rim production. For example, tochilinite and phyllosilicates commonly form rims around matrix carbonates, which are generally believed to have precipitated from alteration fluids on the CM parent body. This suggests that the rims surrounding matrix carbonates may also have been produced by alteration processes. Partially replaced chondrule olivines bear a striking resemblance to many rimmed olivines in the matrix which suggests, by analogy, that site-specific precipitation of S-bearing phases may also be responsible for the occurrence of many tochilinite-rich rims around isolated matrix olivines. Non-silicate rims precipitate around olivines of any composition, but the process is most effective for fayalitic olivines. Most of the remaining olivines in CM chondrites are relatively Mg-rich, which suggests that the precipitation of S-bearing rims on olivines may not have been an important process in the aqueous alteration of CM chondrites. We conclude that: (1) precursor rim materials in CM chondrites were subjected to pervasive aqueous alteration on the CM parent body; and (2) textures and mineral associations observed in CM chondrites also suggest the possibility of in situ rim production.

Formation of thin sulfide rinds on the CM parent body. [Abstract only

NASA Technical Reports Server (NTRS)

Browning, L. B.; Mcsween, H. Y., Jr.; Zolensky, M.

1994-01-01

Many of the textures that are observed in CM chondrites have been alternately assigned nebular, parent-body, or combined nebular-parent body origins. Since it is very difficult to substantiate the production of complex textures in the nebula, an alternate approach to this problem is to rigorously determine which of the observable textures could have been produced by reasonable aqueous alteration processes on the CM parent body. Potential parent body reactions involving S deserve special attention because S-bearing phase define many important CM textures, such as rims. We have examined the possibility that the thin (about 5 microns) rinds of sulfides observed around some partially dissolved olivines within the chondrules and matrixes of CM chondrites were formed by the preferential precipitation of sulfides at or near dissolving olivine boundaries during parent-body alteration. Our model defines two infinite and parallel planes of olivine that are separated by pure water. Average separation distances between olivine grains in CM chondrites at the time of accretion (about 100-200 microns) were estimated by assuming a closed system fluid/rock ratio of 45% and varying the bimodal grain-size distribution. We restrict our calculations to the case of an isochemical system with sufficient bisulfide in solution to account for precipitation of pyrrhotite at STP. Our model examines the possibility that dissolving olivines with compositions between Fo(sub 0.9) and Fo(sub 0.4) can produce a strong gradient of Fe(2+) at pHs from 7 to 12 such that the precipitation of pyrrhotite will be initiated at the olivine-fluid boundary. Since CM phase equilibria is consistent with highly reducing conditions, Fe released by olivines would largely remain in solution as Fe(2+) until the solubility product of a Fe(2+) bearing phase was exceeded. Our calculations indicate that all examined combinations of olivine composition and pH yield a strong Fe(2+) gradient at the time the pyrrhotite solubility is exceeded near the olivine-fluid boundary. This favors the initiation of sulfide precipitation around dissolving olivines. However, sulfide rinds are not observed around all partially dissolved olivine grains in CM chondrites, which suggests that the availability of aqueous sulfide species limits the production of the thin sulfide rinds.

Reconstructing the thermal evolution of the CK chondrite parent body using Northwest Africa 5343, the least metamorphosed CK chondrite

NASA Astrophysics Data System (ADS)

Dunn, T. L.; Gross, J.; O'Hara, E. J.

2017-12-01

Carbonaceous chondrites (CCs) represent some of the most pristine solar system material, providing constraints on the early formation of planetesimals. The CK chondrites are the only group of CCs to exhibit the full range of thermal metamorphism (petrologic type 3 to 6). Most unequilibrated CK chondrites (CK3s) have been metamorphosed to petrologic subtype 3.8 or higher. However, homogeneity of olivine suggests that CK3 chondrite Northwest Africa (NWA) 5343 is less metamorphosed than the other CK3s. The presence of unrecrystallized matrix indicates that it is less than petrologic type 3.7. To better assess the lower limits of metamorphism on the CK chondrite parent body, we performed a detailed analysis of matrix material in NWA 5343. Ascertaining the lower limit of metamorphism in the CK chondrites is critical when addressing the CK-CV parent body debate (e.g., one vs. two parent bodies), and will shed light onto the evolution of metamorphosed CC parent bodies. We recognize two texturally distinct regions in the matrix of NWA 5343. Both have similar mineralogies (mostly olivine with lesser pyroxene and plagioclase), but differ in grain size, shape, and porosity. The porous region of the sample is characterized by subhedral-rounded olivine grains, typically < 40 µms, surrounded by empty pore space ( 10-14% porosity). Some small patches of matrix within the porous region contain angular olivine grains that are < 10 µms, similar to "clastic matrix" typically observed in some low petrologic type CCs and ordinary chondrites (OCs). In the glassy matrix region of NWA 5343 (3-7% porosity), olivine grains are larger (20-40 µms) and more anhedral. Skeletal pyroxene is also common. Original pore space is filled with a Ca-rich glass that appears to originate from an unusual vein in this region. Most interestingly, the extent of metamorphism varies within NWA 5343. Larger, anhedral olivine in the glassy region suggest that this region is more metamorphosed than the porous region. Even within the porous region there is a range of metamorphism, with small patches of granoblastic olivine intermixed with the clastic matrix. This suggests that NWA 5343 may represent a metamorphic breccia, a common occurrence in OCs and CCs of lower petrologic types, and provides insight into the evolution of the only completely metamorphosed CC parent body.

The use of the nest for parental roosting and thermal consequences of the nest for nestlings and parents.

PubMed

Nilsson, Jan-Åke; Nord, Andreas

2017-01-01

At temperate latitudes, altricial birds and their nestlings need to handle night temperatures well below thermoneutrality during the breeding season. Thus, energy costs of thermoregulation might constrain nestling growth, and low nocturnal temperatures might require resources that parents could otherwise have invested into nestlings during the day. To manipulate parental work rate, we performed brood size manipulations in breeding marsh tits ( Poecile palustris ). Nest box temperatures were always well above ambient temperature and increased with increasing brood size. In line with predictions, a large majority of females (but no males) made use of this benign environment for roosting. Furthermore, females tending enlarged broods, thereby having to work harder during the day, reduced their body temperature at night. This might have reduced nocturnal energy expenditure. Our finding that a higher proportion of enlarged, as compared to control, females continued to use the nest box as roosting sites even after a simulated predation event despite increased vulnerability to predation, further highlighting the need for energy conservation in this group. High nest box attendance and reduced body temperature in brood-reduced females may indicate that these females prioritised self-maintenance by initiating other costly physiological adjustments, e.g. moult, when relieved from parental work. We suggest that the energy demand for defending homeothermy is an element of the general trade-off between current and future reproduction, i.e. between daytime investment in food provisioning and the potential short- and long-term costs of a reduction in body temperature and increased predation risk. Even during summer at temperate latitudes, breeding birds need to use energy to maintain stable body temperature. Parents, thus, need to enter the night with sufficient body reserves to cover energy requirements for thermoregulation. As these resources could be used for feeding nestling during the day, adaptations to reduce the cost of thermoregulation would be selected for. We performed brood size manipulations, thereby increasing the need for nestling provisioning in marsh tits ( Parus palustris ). We found that females typically spent the night in the thermally benign environment of the nest box together with their brood. Females working hard during the day continued to roost in the nest box during the night despite an increase in the perceived risk of nest predation. Furthermore, these females reduced their body temperature at night, thereby reducing the gradient between ambient and body temperature, further reducing the cost of thermoregulation.

Validity of parent-reported weight and height of preschool children measured at home or estimated without home measurement: a validation study

PubMed Central

2011-01-01

Background Parental reports are often used in large-scale surveys to assess children's body mass index (BMI). Therefore, it is important to know to what extent these parental reports are valid and whether it makes a difference if the parents measured their children's weight and height at home or whether they simply estimated these values. The aim of this study is to compare the validity of parent-reported height, weight and BMI values of preschool children (3-7 y-old), when measured at home or estimated by parents without actual measurement. Methods The subjects were 297 Belgian preschool children (52.9% male). Participation rate was 73%. A questionnaire including questions about height and weight of the children was completed by the parents. Nurses measured height and weight following standardised procedures. International age- and sex-specific BMI cut-off values were employed to determine categories of weight status and obesity. Results On the group level, no important differences in accuracy of reported height, weight and BMI were identified between parent-measured or estimated values. However, for all 3 parameters, the correlations between parental reports and nurse measurements were higher in the group of children whose body dimensions were measured by the parents. Sensitivity for underweight and overweight/obesity were respectively 73% and 47% when parents measured their child's height and weight, and 55% and 47% when parents estimated values without measurement. Specificity for underweight and overweight/obesity were respectively 82% and 97% when parents measured the children, and 75% and 93% with parent estimations. Conclusions Diagnostic measures were more accurate when parents measured their child's weight and height at home than when those dimensions were based on parental judgements. When parent-reported data on an individual level is used, the accuracy could be improved by encouraging the parents to measure weight and height of their children at home. PMID:21736757

Petrology of a nonindigenous microgranitic clast in polymict ureilite EET 87720: Evidence for formation of evolved melt on an unknown parent body

NASA Astrophysics Data System (ADS)

Beard, A. D.; Downes, H.; Chaussidon, M.

2015-09-01

EET 87720 is a polymict ureilite breccia known to contain numerous nonindigenous fragments. We have discovered a microgranitic clast in an interior chip of Elephant Moraine (EET) 87720. The clast consists of a granophyre-like intergrowth of a pure SiO2 phase (tridymite) and albite, mantling a zoned oligoclase phenocryst. In the intergrowth, the tridymite occurs as thin elongate vermicular blebs within larger albite crystals. The granophyre-like intergrowth and the oligoclase phenocryst share a common margin, suggesting that the clast was originally part of a larger fragment. An estimate of its bulk composition is equivalent to that of granite (77 wt% SiO2). Patches of high-Si K-bearing glass occur interstitially within the clast; they have high concentrations of SO3 (11-12 wt%) and contain Cl (0.6 wt%), suggesting that the clast formed on a volatile-rich parent body perhaps resembling early Mars. The mean oxygen isotope composition of the feldspar and tridymite in the clast is very different from the oxygen isotope compositions of ureilites, and is similar to those of silicate inclusions in IIE and IVA irons. Thus, the clast is not indigenous to the ureilite parent body, but it provides evidence for the formation of evolved melts on an unknown parent body in the early solar system.

Internationally Adopted Children: Important Information for Parents

MedlinePlus

... Size Email Print Share Internationally Adopted Children: Important Information for Parents Page Content Article Body Congratulations on ... with whom your child may have contact. Important Information for Your Child’s Doctor: Children adopted internationally often ...

Iron-Deficiency Anemia (For Parents)

MedlinePlus

... Videos for Educators Search English Español Iron-Deficiency Anemia KidsHealth / For Parents / Iron-Deficiency Anemia What's in ... common nutritional deficiency in children. About Iron-Deficiency Anemia Every red blood cell in the body contains ...

When Your Parents Fight (For Kids)

MedlinePlus

... First Aid & Safety Doctors & Hospitals Videos Recipes for Kids Kids site Sitio para niños How the Body ... from a job or other worries. How Do Kids Feel When Their Parents Fight? Kids usually feel ...

Efficacy of a Self-Administered Home-Based Parent Intervention on Parenting Behaviors for Preventing Adolescent Substance Use

ERIC Educational Resources Information Center

Griffin, Kenneth W.; Samuolis, Jessica; Williams, Christopher

2011-01-01

A growing body of literature suggests that parenting practices characterized by careful monitoring, firm and consistent limit setting, and nurturing communication patterns with children are protective against adolescent substance use and other problem behaviors. Family-based prevention programs that promote these behaviors can be an effective way…

The Helicopter Parent: Research toward a Typology (Part I)

ERIC Educational Resources Information Center

Somers, Patricia; Settle, Jim

2010-01-01

With 117,000 hits on a recent Google[TM] search, the phenomenon of helicopter parenting has been widely reported in the popular press. Yet the scholarly literature is anemic on the topic. This article, part one of a two-part series, presents the small body of research on helicopter parenting and describes a qualitative study of 190 participants…

Seeking a "Critical Mass": Middle-Class Parents' Collective Engagement in City Public Schooling

ERIC Educational Resources Information Center

Posey-Maddox, Linn; Kimelberg, Shelley McDonough; Cucchiara, Maia

2016-01-01

A growing body of literature has begun to explore the individual identities, motivations, and school choices of middle-class, typically white, parents who choose to reside in socioeconomically and racially mixed central city neighborhoods. Drawing on qualitative research in three US cities, we argue that a focus on middle-class parents' collective…

The Longitudinal Impact of Distal, Non-Familial Relationships on Parental Monitoring: Implications for Delinquent Behavior

ERIC Educational Resources Information Center

Jaggers, Jeremiah W.; Bolland, Anneliese C.; Tomek, Sara; Bolland, Kathleen A.; Hooper, Lisa M.; Church, Wesley T., II; Bolland, John M.

2018-01-01

An extensive body of work shows that parental monitoring reduces the likelihood of risky behaviors among youth, yet little attention has been given to the factors compelling parents to engage in monitoring behaviors. The current study examines the association between non-familial, adolescent relationships (i.e., school connectedness, community…

Adolescent Perceptions of School Safety for Students with Lesbian, Gay, Bisexual, and Transgender Parents

ERIC Educational Resources Information Center

Russell, Stephen T.; McGuire, Jenifer K.; Lee, Sun-A; Larriva, Jacqueline C.; Laub, Carolyn

2008-01-01

A growing body of research indicates that lesbian, gay, bisexual, and transgender (LGBT) students are often unsafe at school. Little research has examined school safety for students with LGBT parents. We examined adolescents' perceptions of school safety for students with LGBT parents using data from a survey of 2,302 California sixth through…

Helicopter Parents of Community College Students: How Community College Professionals Operationally Define and Address This Phenomenon

ERIC Educational Resources Information Center

Hightower, Helen C.

2014-01-01

This study examined whether the phenomenon of "parental over-involvement" occurred in the Virginia Community College System. Concern has been expressed in the popular and academic literature in recent years over the increased level of parental involvement at four year institutions whose student bodies consist almost exclusively of…

Child Sexual Abuse Prevention: Psychoeducational Groups for Preschoolers and Their Parents

ERIC Educational Resources Information Center

Kenny, Maureen

2009-01-01

Teaching parents and their young children about ways to avoid harm can be accomplished with much success in a group setting. Parents as Teachers of Safety (PaTS) is a multi-family educational group which instructs families on environmental and personal body safety rules, with an emphasis on improving knowledge and skills related to sexual abuse…

Adolescent Boys' Grooming Product Use and Perceived Health Risks: An Exploration of Parental Influence

ERIC Educational Resources Information Center

Yoo, Jeong-Ju; Jacob, John; Baier, Margaret

2012-01-01

Objective: To investigate parental influence on adolescent boys' use and risk-perceptions of using appearance-related products. Design: Using appearance-enhancing products can present a health threat to adolescents, as these products are not only applied to the body, but can also be ingested. Adolescents may look to their parents for information…

Parenting in the Age of High-Stakes Testing: Gifted and Talented Admissions and the Meaning of Parenthood

ERIC Educational Resources Information Center

Roda, Allison

2017-01-01

Background/Context: This work contributes to the growing body of scholarly and popular literature on middle-class parental anxiety and competition to ensure their children's academic success. Specifically, this study provides a better understanding of the measures parents will take to obtain high status gifted and talented (G&T) placements…

Emotion Dysregulation and Loss-of-Control Eating in Children and Adolescents

PubMed Central

Kelly, Nichole R.; Tanofsky-Kraff, Marian; Vannucci, Anna; Ranzenhofer, Lisa M.; Altschul, Annie M.; Schvey, Natasha A.; Shank, Lisa M.; Brady, Sheila M.; Galescu, Ovidiu; Kozlosky, Merel; Yanovski, Susan Z.; Yanovski, Jack A.

2016-01-01

Objective To examine the associations among self-reported loss-of-control (LOC) eating, emotion dysregulation, body mass, and objective energy intake among youth. Emotion dysregulation may be one individual factor that promotes excess energy intake and increases in body mass among youth with LOC eating. Methods Children and adolescents (N=230; 8 to 17 years) enrolled in a non-intervention study completed a structured interview to determine the presence or absence of self-reported LOC eating. Children’s emotion dysregulation was assessed via parent-report with the Child Behavior Checklist. Youth also completed two test meals to capture “binge” and “normal” eating. Body composition was examined using air displacement plethysmography. Results After controlling for relevant covariates, youth with self-reported LOC eating had higher parent-reported emotion dysregulation than those without LOC. Parent-reported emotion dysregulation was also associated with greater observed energy intake (after accounting for body mass), as well as higher fat mass. Emotion dysregulation also moderated associations between LOC status/sex and body mass variables; among youth with self-reported LOC eating and girls, those with high parent-described emotion dysregulation (versus low) had significantly higher fat mass and BMIz. Conclusions Data from the current study suggest that emotion dysregulation may play a role in energy intake and obesity, particularly among youth with self-reported LOC eating and girls. Additional studies are needed to identify the prospective mechanisms linking poor emotion regulation and LOC eating. These mechanisms, in turn, may inform future interventions targeting excess energy intake and obesity in pediatric samples. PMID:27505194

A new social-family model for eating disorders: A European multicentre project using a case-control design.

PubMed

Krug, Isabel; Fuller-Tyszkiewicz, Matthew; Anderluh, Marija; Bellodi, Laura; Bagnoli, Silvia; Collier, David; Fernandez-Aranda, Fernando; Karwautz, Andreas; Mitchell, Sarah; Nacmias, Benedetta; Ricca, Valdo; Sorbi, Sandro; Tchanuria, Kate; Wagner, Gudrun; Treasure, Janet; Micali, Nadia

2015-12-01

To examine a new socio-family risk model of Eating Disorders (EDs) using path-analyses. The sample comprised 1264 (ED patients = 653; Healthy Controls = 611) participants, recruited into a multicentre European project. Socio-family factors assessed included: perceived maternal and parental parenting styles, family, peer and media influences, and body dissatisfaction. Two types of path-analyses were run to assess the socio-family model: 1.) a multinomial logistic path-model including ED sub-types [Anorexia Nervosa-Restrictive (AN-R), AN-Binge-Purging (AN-BP), Bulimia Nervosa (BN) and EDNOS)] as the key polychotomous categorical outcome and 2.) a path-model assessing whether the socio-family model differed across ED sub-types and healthy controls using body dissatisfaction as the outcome variable. The first path-analyses suggested that family and media (but not peers) were directly and indirectly associated (through body dissatisfaction) with all ED sub-types. There was a weak effect of perceived parenting directly on ED sub-types and indirectly through family influences and body dissatisfaction. For the second path-analyses, the socio-family model varied substantially across ED sub-types. Family and media influences were related to body dissatisfaction in the EDNOS and control sample, whereas perceived abusive parenting was related to AN-BP and BN. This is the first study providing support for this new socio-family model, which differed across ED sub-types. This suggests that prevention and early intervention might need to be tailored to diagnosis-specific ED profiles. Copyright © 2015 Elsevier Ltd. All rights reserved.

Effects of Enhancing School-Based Body Mass Index Screening Reports with Parent Education on Report Utility and Parental Intent To Modify Obesity Risk Factors.

PubMed

Bailey-Davis, Lisa; Peyer, Karissa L; Fang, Yinan; Kim, Jae-Kwang; Welk, Greg J

2017-04-01

School-based body mass index screenings (SBMIS) have been controversial. We aimed to determine if parents would indicate improved utility with SBMIS when the report included parent education and whether parental intent to modify obesity risk factors would vary with report type or child weight. A cluster-controlled trial was conducted with 31 elementary schools randomized to distribute a standard SBMIS report or the standard report plus education (SBMIS+). A random subsample of parents completed a mailed survey (731 SBMIS, 738 SBMIS+). Using a two-stage cluster sampling design, logistic regression models with school-level random effect were used to assess differences between conditions and by weight category. Parents in the SBMIS+ condition vs. the standard condition were more likely to indicate that the report provided useful information (not significant) and an intent to help their child get enough sleep (p < 0.001). Parents of children who were overweight or obese were less likely than parents of children who were not to indicate that the report provided useful information about their child's weight status (p < 0.001) or access to resources (p < 0.05). However, these parents were more likely to plan a visit to healthcare provider (p < 0.001) and to intend to limit sugar-sweetened beverages (p < 0.05). Parental education can enhance the utility of the SBMIS report and parental intention to modify at least one obesity risk factor. SBMIS reports prompted parents of children with overweight and obesity to seek clinical care and limit sugar-sweetened drinks.

Dietary intake and nutritional status of vegetarian and omnivorous preschool children and their parents in Taiwan.

PubMed

Yen, Chin-En; Yen, Chi-Hua; Huang, Men-Chung; Cheng, Chien-Hsiang; Huang, Yi-Chia

2008-07-01

The aim of this study was to assess and compare dietary intake and nutritional status of vegetarian and omnivorous preschool children and their parents. Fifty-six omnivores (28 children and 28 parents) and 42 vegetarians (21 preschool children with 18 lacto-ovo-vegetarians and 3 ovo-vegetarians; 21 parents with 16 lacto-ovo-vegetarians, 2 ovo-vegetarians, 1 lacto-vegetarian, and 2 vegans) were recruited. Anthropometric measurements were taken; body mass index and weight-for-height index (WHI) were calculated. Nutrient intake was recorded using 3-day dietary records. Fasting venous blood samples were obtained to estimate hematologic and vitamin status parameters. Height, weight, body mass index, WHI, and triceps skinfold thickness value differences between omnivores and vegetarians in both parent and child groups were not found. Both omnivorous parents and their children had significantly higher fat and lower fiber intakes than vegetarian parents and children. Omnivorous children had significantly higher protein and lower vitamin C intakes than vegetarian children, whereas omnivorous parents had significantly lower vitamin A and iron intakes than vegetarian parents. Vegetarians and omnivores in both parent and child groups had mean calcium consumption less than 75% of the Taiwan dietary intakes. All mean hematologic and biochemical nutrient status indices were within the reference range in any groups. However, both vegetarian parents and children had significantly lower mean total cholesterol and serum ferritin concentrations than those of omnivorous parents and children. Our vegetarian and omnivorous preschool children had normal growth and adequate nutritional status. However, both parents and children had inadequate calcium intakes, which may potentially affect bone health, especially for preschool children in the growing stage.

Role of obesity and media in body weight concern among female university students in Kuwait.

PubMed

Musaiger, Abdulrahman O; Al-Mannai, Mariam

2013-04-01

The aim of this study was to find out the association of media and obesity status with body weight concern among female university students in Kuwait. 228 female students, aged 19-25 years, were selected at convenience from the Women's College in Kuwait. A previously validated questionnaire was used to collect information on the role of media in body concern and how parents, peers and the girls themselves perceived girls' body shapes. Weight and height were gathered by self-reporting. Use of internet and reading women's magazines had a significant impact on dieting by the girls to lose weight (P<0.0007 and P<0.0114, respectively). The mass media had two to three times more influence on obese girls than non-obese girls. Only watching television had a significant impact on girls' body shape concern (P<0.053). About 30% of non-obese and 81% of obese girls were dissatisfied with their current weight. There were significant differences between obese and non-obese girls regarding the girls' views and the views of their peers and parents about the body weight of the girls (P<0.000 for all). The pressure from peers and parents, in addition to the mass media, may lead to disturbed attitudes towards eating among Kuwaiti girls. Copyright © 2012 Elsevier Ltd. All rights reserved.

Assessing the Landscape: Body Image Values and Attitudes among Middle School Boys and Girls

ERIC Educational Resources Information Center

Grosick, Tracy L.; Talbert-Johnson, Carolyn; Myers, Melissa J.; Angelo, Renee

2013-01-01

Background: Body image refers to an individual's thoughts and feelings about his or her body and physical appearance. To date, several qualitative and quantitative findings implicate sociocultural influences, such as the media or parental pressure, in shaping female adolescents' body image perceptions. Overall, there is not much quantitative…

Health-related quality of life of Spanish children with cystic fibrosis.

PubMed

Groeneveld, Iris F; Sosa, Elena S; Pérez, Margarita; Fiuza-Luces, Carmen; Gonzalez-Saiz, Laura; Gallardo, Cristian; López-Mojares, Luis M; Ruiz, Jonatan R; Lucia, Alejandro

2012-12-01

To investigate (1) the contributions of sex, age, nutritional status- and physical-fitness-related variables on health-related quality of life (HRQOL) in Spanish children with cystic fibrosis, and (2) the agreement on HRQOL between children and their parents. In 28 children aged 6-17 years, body mass index percentile, percentage body fat, physical activity, pulmonary function, cardiorespiratory fitness, functional mobility, and dynamic muscle strength were determined using objective measures. HRQOL was measured using the revised version of the cystic fibrosis questionnaire. Simple and multiple linear regression analyses were performed to determine the variables associated with HRQOL. To assess the agreement on HRQOL between children and parents, intra-class correlation coefficients (ICCs) were calculated. Girls reported worse emotional functioning, a higher treatment burden, and more respiratory problems than boys. Greater functional mobility appeared associated with a less favourable body image and more eating disturbances. Agreement on HRQOL between children and parents was good to excellent, except for the domain of treatment burden. Sex and age were stronger predictors of HRQOL than nutritional status- or physical-fitness-related variables. Children reported a lower treatment burden than their parents perceived them to have.

Organized sports, overweight, and physical fitness in primary school children in Germany.

PubMed

Drenowatz, Clemens; Steiner, Ronald P; Brandstetter, Susanne; Klenk, Jochen; Wabitsch, Martin; Steinacker, Jürgen M

2013-01-01

Physical inactivity is associated with poor physical fitness and increased body weight. This study examined the relationship between participation in organized sports and overweight as well as physical fitness in primary school children in southern Germany. Height, weight, and various components of physical fitness were measured in 995 children (7.6 ± 0.4 years). Sports participation and confounding variables such as migration background, parental education, parental body weight, and parental sports participation were assessed via parent questionnaire. Multiple logistic regression as well as multivariate analysis of covariance (MANCOVA) was used to determine associations between physical fitness, participation in organized sports, and body weight. Participation in organized sports less than once a week was prevalent in 29.2%, once or twice in 60.2%, and more often in 10.6% of the children. Overweight was found in 12.4% of the children. Children participating in organized sports more than once per week displayed higher physical fitness and were less likely to be overweight (OR  =  0.52, P < 0.01). Even though causality cannot be established, the facilitation of participation in organized sports may be a crucial aspect in public health efforts addressing the growing problems associated with overweight and obesity.

Improving uptake and engagement with child body image interventions delivered to mothers: Understanding mother and daughter preferences for intervention content.

PubMed

Garbett, Kirsty M; Diedrichs, Phillippa C

2016-12-01

Mothers are a key influence on adolescent girls' body image. This study aimed to improve understanding of mothers' and daughters' preferences for content in body image interventions designed to assist mothers to promote positive body image among their daughters. British mother-daughter dyads (N=190) viewed descriptions of five evidence-based influences on body image (family, friends, and relationships; appearance-based teasing; media and celebrities; appearance conversations; body acceptance and care). Mothers and daughters each selected the two most important influences to learn about in these interventions. Overall, both mothers and daughters most frequently opted for family, friends, and relationships and body acceptance and care, whereas media and celebrities was their least preferred topic. While the overall sample of mothers and daughters agreed on preferences, Fisher's exact tests showed that within-dyad agreement was low. Recommendations for improving parent and child engagement with, and effectiveness of, child body image interventions delivered to parents are discussed. Copyright © 2016 Elsevier Ltd. All rights reserved.

Effects of geolocation archival tags on reproduction and adult body mass of sooty shearwaters (Puffinus griseus)

USGS Publications Warehouse

Adams, J.; Scott, D.; McKechnie, S.; Blackwell, G.; Shaffer, S.A.; Moller, H.

2009-01-01

We attached 11 g (1.4% body-mass equivalent) global location sensing (GLS) archival tag packages to tarsi of 25 breeding sooty shearwaters (Puffinus griseus, titi) on Whenua Hou (Codfish Island), New Zealand during the chick-rearing period in 2005. Compared with chicks reared by non-handled adults that did not carry tags, deployment of tags on one or both adult parents ultimately resulted in 35% reduction in chick body mass and significantly reduced chick skeletal size preceding fledging (19 April). However, body mass between chick groups was not significantly different after controlling for skeletal size. Effects on chicks were more pronounced in six pairs where both parents carried tags. Chick mass was negatively related to the duration that adults carried tags. In this study, none of the chicks reared by pairs where both parents were tagged, 54% of chicks reared by pairs where one parent was tagged, and 83% of chicks reared by non-handled and non-tagged parents achieved a previously determined pre-fledging mass threshold (564 g; Sagar & Horning 1998). Body mass of adults carrying tags and returning from transequatorial migration the following year were 4% lighter on average than non-tagged birds, but this difference was not statistically significant. Reduced mass among chicks reared by adults carrying tags during the chick-provisioning period indicated that adults altered "normal" provisioning behaviours to maintain their own body condition at the expense of their chicks. Population-level information derived from telemetry studies can reveal important habitat-linked behaviours, unique aspects of seabird foraging behaviours, and migration ecology. Information for some species (e.g., overlap with fisheries) can aid conservation and marine ecosystem management. We advise caution, however, when interpreting certain data related to adult provisioning behaviours (e.g., time spent foraging, provisioning rates, etc.). If effects on individuals are of concern, we suggest shorter-term deployments, smaller and lighter tags, and alternative attachment techniques, especially when investigating threatened or endangered species. ?? The Royal Society of New Zealand 2009.

Stress in childhood

MedlinePlus

... body changes, in both boys and girls Seeing parents go through a divorce or separation Money problems in the family Living in an unsafe home or neighborhood SIGNS OF UNRESOLVED STRESS IN ... lead parents to suspect an increased stress level is present. ...

Couch kids: correlates of television viewing among youth.

PubMed

Gorely, Trish; Marshall, Simon J; Biddle, Stuart J H

2004-01-01

The purpose of this study was to review the published empirical correlates of television/video viewing among youth (2 to 18 years). A descriptive semi-quantitative review was conducted based on 68 primary studies. Variables consistently associated with TV/video viewing were ethnicity (non-white +), parent income (-), parent education (-), body weight (+), between meal snacking (+), number of parents in the house (-), parents TV viewing habits (+), weekend (+) and having a TV in the bedroom (+). Variables consistently unrelated to TV/video viewing were sex, other indicators of socio-economic status, body fatness, cholesterol levels, aerobic fitness, strength, other indicators of fitness, self-perceptions, emotional support, physical activity, other diet variables, and being an only child. Few modifiable correlates have been identified. Further research should aim to identify modifiable correlates of TV/video viewing if interventions are to be successfully tailored to reduce this aspect of inactivity among youth.

Rotational spectral variations of asteroid (8) Flora Implications for the nature of the S-type asteroids and for the parent bodies of the ordinary chondrites

NASA Technical Reports Server (NTRS)

Gaffey, M. J.

1984-01-01

The surface material and the surface material heterogeneities of the asteroid Flora are characterized using the best available data sets and the most sophisticated interpretive calibrations. Five spectrally derived mineralogic and patrologic properties of the surface assemblage of Flora which are relevant to whether this body is a differentiated or undifferentiated object are considered: bulk mineralogy, mafic mineral assemblage, metallic phase, pyroxene composition and structural type, and mineralogic variation. All of these properties indicate that Flora is a differentiated body. Flora is probably the residual core of an intensely heated, thermally evolved, and magnetically differentiated planetesimal which was subsequently disrupted. The present surface sample layers formed at or near the core-mantle boundary in the parent body.

Health information sources accessed by college females: differences between body-image distorted and non-body-image distorted.

PubMed

Nustad, Jill; Adams, Troy; Moore, Monique

2008-01-01

This study examined and compared sources of health-related information accessed by female college students with and without body image distortions, and the believability of those sources. Survey data from the American College Health Association, National College Health Assessment were studied retrospectively (N = 27,648). Body image distorted (BID) and non-BID students' most frequent health information sources were parents (76.1% BID; 77.1% non-BID) and internet (70.3% BID; 69.5% non-BID). Believability was greatest for health educators (90.6% BID; 91.1% non-BID) and lowest for television (14.4% BID; 14.5% non-BID). Health intervention strategies for college women should market to parents and teach recognition of credible internet sources of health information.

Surgical repair of pectus excavatum markedly improves body image and perceived ability for physical activity: multicenter study.

PubMed

Kelly, Robert E; Cash, Thomas F; Shamberger, Robert C; Mitchell, Karen K; Mellins, Robert B; Lawson, M Louise; Oldham, Keith; Azizkhan, Richard G; Hebra, Andre V; Nuss, Donald; Goretsky, Michael J; Sharp, Ronald J; Holcomb, George W; Shim, Walton K T; Megison, Stephen M; Moss, R Lawrence; Fecteau, Annie H; Colombani, Paul M; Bagley, Traci; Quinn, Amy; Moskowitz, Alan B

2008-12-01

This study evaluated changes in both physical and psychosocial quality of life reported by the parent and child after surgical repair of pectus excavatum. As part of a multicenter study of pectus excavatum, a previously validated tool called the Pectus Excavatum Evaluation Questionnaire was administered by the research coordinator, via telephone, to parents and patients (8-21 years of age) before and 1 year after surgery. Eleven North American children's hospitals participated. From 2001 to 2006, 264 patients and 291 parents completed the initial questionnaire, and 247 patients and 274 parents completed the postoperative questionnaire. Responses used a Likert-type scale of 1 to 4, reflecting the extent or frequency of a particular experience, with higher values conveying less-desirable experience. Preoperative psychosocial functioning was unrelated to objective pectus excavatum severity (computed tomographic index). Patients and their parents reported significant positive postoperative changes. Improvements occurred in both physical and psychosocial functioning, including less social self-consciousness and a more-favorable body image. For children, the body image component improved from 2.30+/-0.62 (mean+/-SD) to 1.40+/-0.42 after surgery and the physical difficulties component improved from 2.11+/-0.82 to 1.37+/-0.44. For the parent questionnaire, the child's emotional difficulties improved from 1.81+/-0.70 to 1.24+/-0.36, social self-consciousness improved from 2.86+/-1.03 to 1.33+/-0.68, and physical difficulties improved from 2.14+/-0.75 to 1.32+/-0.39. Ninety-seven percent of patients thought that surgery improved how their chest looked. Surgical repair of pectus excavatum can significantly improve the body image difficulties and limitations on physical activity experienced by patients. These results should prompt physicians to consider the physiologic and psychological implications of pectus excavatum just as they would any other physical deformity known to have such consequences.

Thermal Studies of Ammonium Cyanide Reactions: A Model for Thermal Alteration of Prebiotic Compounds in Meteorite Parent Bodies

NASA Technical Reports Server (NTRS)

Hammer, P. G.; Locke, D. R.; Burton, A. S.; Callahan, M. P.

2017-01-01

Organic compounds in carbonaceous chondrites were likely transformed by a variety of parent body processes including thermal and aqueous processing. Here, we analyzed ammonium cyanide reactions that were heated at different temperatures and times by multiple analytical techniques. The goal of this study is to better understand the effect of hydrothermal alteration on cyanide chemistry, which is believed to be responsible for the abiotic synthesis of purine nucleobases and their structural analogs detected in carbonaceous chondrites.

Parent-Body Modification of Chondritic Meteorites

NASA Technical Reports Server (NTRS)

Rubin, Alan

2003-01-01

This proposal focused on the parent-body modification of chondritic materials and substantial progress was made in the last year. A summary of the work accomplished during this period is discussed. The topics include: 1) Chromite-Plagioclase Assemblages in Ordinary Chondrites; 2) The Gujba Bencubbin-like meteorite fall; 3) NWA428: A rock that Experienced Impact-induced Annealing; 4) Spade: An Annealed H-chondrite Impact-melt Breccia; and 5) Post-shock Annealing in Ordinary Chondrites. A list of the papers submitted or published during the period is also presented.

Penecontemporaneous metamorphism, fragmentation, and reassembly of ordinary chondrite parent bodies

NASA Technical Reports Server (NTRS)

Grimm, R. E.

1985-01-01

The thermal histories of ordinary chondrites and the canonical internal heating or onion shell models, which predict an inverse relation between the petrologic type of chondrites and the metallographic cooling rate, are reviewed. The thermal and accretional requirements of the 'metamorphosed planetesimal' model proposed by Scott and Rajan (1981) are analyzed, and an alternative model consistent with the metallographic cooling rate constraints is suggested in which ordinary chondrite parent bodies are collisionally fragmented and then rapidly reassembled before metamorphic heat has been dissipated.

Textural constraints on the formation of alteration phases in CM chondrites

NASA Technical Reports Server (NTRS)

Joseph, L. H.; Browning, L. B.; Zolensky, M. E.

1994-01-01

Although it is generally believed that the secondary alteration phases observed in CM chondrites resulted from parent body reactions, the influence of nebular processing can not yet be dismissed. We have analyzed 5 CM falls using optical and electron microscopy to construct a comprehensive pictorial reference set of textural and mineralogical associations bearing on the origin of alteration products in these meteorites. Our analyses support pervasive aqueous alteration on the CM parent body, but they do not exclude the possibility of minor nebular alteration.

Mineralogy, Petrology, Chronology, and Exposure History of the Chelyabinsk Meteorite and Parent Body

NASA Technical Reports Server (NTRS)

Righter, K.; Abell, P.; Agresti, D.; Berger, E. L.; Burton, A. S.; Delaney, J. S.; Fries, M. D.; Gibson, E. K.; Harrington, R.; Herzog, G. F.;

A Two-Generation Study of Body Mass Index, Energy Balance and Specific Physical Activity of College Students and Their Respective Parents Living in the Same Household at Los Angeles, California, U.S.A.

ERIC Educational Resources Information Center

Liang, Ying; Lee, Judy; Tam, Chick F.; Bridges, Elizabeth; Keating, Xiaofen D.

2007-01-01

The purpose was to compare the differences in body mass index (BMI), energy balance (EB) and specific physical activity (SPA) between 30 CSULA college students (Y) and their respective parents (O) living in the same household at Los Angeles, California, U.S.A. Each student completed a 24-hour dietary record with SPA journal, and the same for…

Comparative Planetary Mineralogy: Basaltic Plagioclase from Earth, Moon, Mars and 4 Vesta

NASA Technical Reports Server (NTRS)

Karner, J. M.; Papike, J. J.; Shearer, C. K.

2003-01-01

Major, minor and trace element analysis of silicates has allowed for the study of planetary basalts in a comparative planetary mineralogy context. We continue this initiative by exploring the chemistry of plagioclase feldspar in basalts from the Earth, Moon, Mars and 4 Vesta. This paper presents new data on plagioclase from six terrestrial basalt suites including Keweenawan, Island Arc, Hawaiian, Columbia Plateau, Taos Plateau, and Ocean Floor; six lunar basalt suites including Apollo 11 Low K, Apollo 12 Ilmenite, Apollo 12 Olivine, Apollo 12 Pigeonite, Apollo 15 Olivine, and Apollo 15 Pigeonite; two basaltic martian meteorites, Shergotty and QUE 94201; and one unequilibrated eucrite, Pasamonte.

Oxygen isotope variation in stony-iron meteorites.

PubMed

Greenwood, R C; Franchi, I A; Jambon, A; Barrat, J A; Burbine, T H

2006-09-22

Asteroidal material, delivered to Earth as meteorites, preserves a record of the earliest stages of planetary formation. High-precision oxygen isotope analyses for the two major groups of stony-iron meteorites (main-group pallasites and mesosiderites) demonstrate that each group is from a distinct asteroidal source. Mesosiderites are isotopically identical to the howardite-eucrite-diogenite clan and, like them, are probably derived from the asteroid 4 Vesta. Main-group pallasites represent intermixed core-mantle material from a single disrupted asteroid and have no known equivalents among the basaltic meteorites. The stony-iron meteorites demonstrate that intense asteroidal deformation accompanied planetary accretion in the early Solar System.

Pairing Among the EET87503 Group of Howardites and Polymict Eucrites

NASA Technical Reports Server (NTRS)

Buchanan, P. C.; Lindstrom, D. J.; Mittlefehldt, D. W.

2000-01-01

The ten HED polymict breccias EET82600, EET87503, EET87509, EET87510, EET87512, EET87513, EET87518, EET87528, EET87531, and EET92022 were found over a broad area in the Elephant Moraine collecting region of Antarctica. Locations are scattered among the Main (Elephant Moraine), Meteorite City, and Texas Bowl icefields and the Northern Ice Patch. It was previously suggested that these polymict breccias are paired. However, degree of terrestrial alteration among these meteorites varies from relatively pristine (type A) to extensively altered (type B/C) and there are textural, mineralogical, and compositional differences. This study is a reevaluation of the pairing of these meteorites.

Pairing Among the EET87503 Group of Howardites and Polymict Eucrites

NASA Technical Reports Server (NTRS)

Buchanan, Paul C.; Lindstrom, D. J.; Mittlefehldt, D. W.

1999-01-01

The ten HED polymict breccias EET82600, EET87503, EET87509, EET87510, EET87512, EET87513, EET87518, EET87528, EET87531, and EET92022 were found over a broad area in the Elephant Moraine collecting region of Antarctica. Locations are scattered among the Main (Elephant Moraine), Meteorite City, and Texas Bowl icefields and the Northern Ice Patch. It was previously suggested that these polymict breccias are paired. However, degree of terrestrial alteration among these meteorites varies from relatively pristine (type A) to extensively altered (type B/C) and there are textural, mineralogical, and compositional differences. This study is a reevaluation of the pairing of these meteorites.