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.

Ti K-edge EXAFS and XANES study on tektites from different strewnfields

NASA Astrophysics Data System (ADS)

Wang, L.; Furuta, T.; Okube, M.; Yoshiasa, A.

2011-12-01

The concentration and local structure of each element may have various kinds of information about the asteroid impact and mass extinction. Farges and Brown have discussed about the Ti local structure by XANES, and concluded that Ti in tektite occupies 4-coordinated site. EXAFS can be analyzed to give precise information about the distance from Ti to near neighbors. The XAFS measurement of Ti local structure was preformed at the beamline 9C of the Photon Factory in KEK, Tsukuba, Japan. The specimens of tektites are from different strewnfields, they are: indochinite, bediasite, hainanite, philippinite, australite and moldavite. Sample for comparison are Libya desert glass and suevite. The k3χ(k) function was transformed into the radial structure function (RSF) for Ti K-edge of six tektites. The RSF for the Ti atom in indochinite and bediasite are similar; hainanite, australite and philippinite are similar; and moldavite is discriminated from others. It indicates that they have the same local atomic environmental around the Ti atoms and extended structure respectively. Coordination numbers and radial structure function are determined by EXAFS analyses (Table 1). We classified the tektites in three types: in indochinite and bediasite, Ti occupies 4-coordinated tetrahedral site and Ti-O distances are 1.84-1.81 Å; in hainanite, australite and philippinite, Ti occupies 5-coordinated trigonal bi-pyramidal or tetragonal pyramidal site and Ti-O distances are 1.92-1.87 Å; in moldavite, Ti occupies the 6-coordinated octahedral site and Ti-O distance is 2.00-1.96 Å. Formation of tektites is related to the impact process. It is generally recognized that tektites were formed under higher temperature and high pressure. But through this study, local structures of Ti are differing in three strewnfields and even different locations of the same strewnfield. What caused the various local structures will be another topic of tektite studies. Local structure of Ti may be changed in the impact event and the following stage. Tektites splashed to the space and travel in several kinds of processes and routes, which lead to different temperature and pressure history. Local structure of Ti should be related with the temperature, pressure, quenching rate, sizes of impact meteorite and size of falling melts. [1] Koeberl. Ann.Rev.Earth Planet.Sci. 14, 323-350 (1986) [2] François Farges & Gordon E. Brown Jr Geochim. Cosmo. Acta.61, 1863-1870 (1997). [3]Paris, E., Dingwell, D., Seifert, F., Mottana, A. & Romano, C. (1994). Phys. Chem. Miner. 21, 520-525.
Table 1 Structure parameters determined by EXAFS

Aerodynamic Evidence Pertaining to the Entry of Tektites into the Earth's Atmosphere

NASA Technical Reports Server (NTRS)

Chapman, Dean R.; Larson, Howard K.; Anderson, Lewis A.

1962-01-01

Evidence is presented which shows that the Australian and Java tektites entered the earth's atmosphere and experienced ablation by severe aerodynamic heating in hypervelocity flight. The laboratory experiments on hypervelocity ablation have reproduced ring-wave flow ridges and coiled circumferential flanges like those found on certain of these tektites. Systematic striae distortions exhibited in a thin layer beneath the front surface of australites also are reproduced in the laboratory ablation experiments, and are shown to correspond to the calculated distortions for aerodynamic ablation of a glass. About 98 percent of Australian tektites represent aerodynamically stable configurations during the ablative portion of an entry trajectory. Certain meteorites exhibit surface features similar to those on tektites.

Fe-57 Moessbauer study of tektites

NASA Technical Reports Server (NTRS)

Evans, B. J.; Leung, L. K.

1976-01-01

Moessbauer measurements were made on selected moldavite, australite, philippinite, and Georgia tektites. The spectra consist of two apparent lines, but at least two quadrupole doublets can be fitted to these spectra. The Moessbauer parameters for these doublets indicate that they arise from Fe2+ ions with local environments, which are relatively rich and relatively poor in calcium, respectively, similar to those in clinopyroxenes. No evidence for Fe3+/Fe2+ ratios above 0.01 (estimated detection limit) have been found in any tektite. Tektites are considerably more reduced than previously believed, and the extent of the reduction shows little or no variation among different types of tektites. These results limit the source materials of tektites to minerals in which the iron is uniformly highly reduced and in which the iron is contained clinopyroxene-like phases.

Lithium in tektites and impact glasses: Implications for sources, histories and large impacts

NASA Astrophysics Data System (ADS)

Magna, T.; Deutsch, A.; Mezger, K.; Skála, R.; Seitz, H.-M.; Mizera, J.; Řanda, Z.; Adolph, L.

2011-04-01

Lithium (Li) abundances and isotope compositions were determined in a representative suite of tektites (moldavites, Muong Nong-type tektites and an australite, Ivory Coast tektites and bediasites), impact-related glasses (Libyan Desert Glass, zhamanshinites and irghizites), a glass fragment embedded in the suevite from the Ries impact crater and sedimentary materials in order to test a possible susceptibility of Li to fractionation during hypervelocity impact events and to de-convolve links to their potential parental sources. The overall data show a large spread in Li abundance (4.7-58 ppm Li) and δ 7Li values (-3.2‰ to 26.0‰) but individual groups of tektites and impact glasses have distinctive Li compositions. Most importantly, any significant high-temperature Li isotope fractionation can be excluded by comparing sedimentary lithologies from central Europe with moldavites. Instead, we suggest that Li isotope compositions in tektites and impact-related glasses are probably diagnostic of the precursor materials and their pre-impact geological histories. The Muong Nong-type tektites and australite specimen are identical in terms of Li concentrations and δ 7Li and we tentatively endorse their common origin in a single impact event. Evidence for low-temperature Rayleigh fractionation, which must have operated prior to impact-induced melting and solidification, is provided for a subset of Muong Nong-type tektites. Although Li isotope variations in most tektites are broadly similar to those of the upper continental crust, Libyan Desert Glass carries high δ 7Li ⩾24.7‰, which appears to mirror the previous fluvial history of parental material that was perhaps deposited in lacustrine environment or coastal seawater. Lithium isotopes in impact-related glasses from the Zhamanshin crater define a group distinct from all other samples and point to melting of chemically less evolved mafic lithologies, which is also consistent with their major and trace element patterns. Extreme shock pressures and the related extreme post-shock temperatures alone appear not to have any effect on the Li isotope systematics; therefore, useful information on parental lithologies and magmatic processes may be retrieved from analyses of Martian and lunar meteorites. Moreover, lack of significant Li depletion in tektites provides further constraints on the loss of moderately volatile elements during the Moon-forming impact.

Neodymium and strontium isotopic study of Australasian tektites - New constraints on the provenance and age of target materials

NASA Technical Reports Server (NTRS)

Blum, Joel D.; Papanastassiou, D. A.; Wasserburg, G. J.; Koeberl, C.

1992-01-01

The Nd and Sr isotopic compositions of Australasian tectites (including two flanged Australian tectites, two low-SiO2 Muong Nong-type tectites, and three high-SiO2 Muong Nong-type tectites) and the Nd, Sm, Sr, and Rb concentrations were investigated by isotope-dilution thermal ionization mass spectrometry, and the Sm-Nd and Rb-Sr isotope systematics were used to study the characteristics of the parental material. It is shown that the Nd and Sr isotopic data provide evidence that all Australasian tektites were derived from a single sedimentary formation with a narrow range of stratigraphic ages close to 170 Ma. It is suggested that all of the Australasian tektites were derived from a single impact event and that the australites represent the upper part of a melt sheet ejected at high velocity, whereas the indochinites represent melts formed at a lower level in the target material distributed closer to the area of the impact.

DARWIN Glass and DARWIN Crater Revisited. Multiple Impacts in the Australasian Strewn Field?

NASA Astrophysics Data System (ADS)

Meisel, T.; Biino, G. G.; Villa, I. M.; Chambers, J. E.; McHone, J. F.

1995-09-01

Darwin glass, an impact glass occurring in South West Tasmania, has been found at least since human beings reached Tasmania ca. 40 k.y. ago. Darwin glass, although in the proximity of the Australasian tektites strewn field, has never been counted as part of it. Darwin Crater was recognized about 30 years ago. Still, the existence of an impact structure in Tasmania has been neglected and does not show up in most compilations of known impact craters. Age determinations on Darwin Glass from the early 70's revealed a combined K-Ar and fission track age of 0.73 +/- 0.04 m.y. [1]. The most recent and most precise estimate for Australites and Indochinites yields 0.784 +/- 0.012 m.y. [2]. The two ages are indistinguishable from each other. This contemporaneity lead to the hypothesis that impact on Earth producing australites also formed Darwin Crater as a primary and/or secondary crater (Gentner et al., 1973). If one believes that all tektites of the Australian strewn field were produced by one impact in or near Indochina, then a special case is required to also form Darwin Crater, which is at least 5000 km away. Atmospheric breakup of a planetary body is a very unlikely possibility, because the distance travelled after breakup is too small to account for the dispersion. Double craters on Earth are always close to each other (e.g., Kara and Kara Ust). A more likely scenario could be an impact of an asteroidal body with an accompanying small moon (e.g., Ida and Gaspra). If one believes in multiple impacts for the formation of Muong Nong-type or layered tektites in the Australasian strewn field, then a collision of an asteroidal body with another body shortly before impact on Earth is required. In this case, an impact on Earth a large distance away (i.e., Tasmania) is realistic. To address the problem of crater recognition and possible simultaneous impact events, a new multidisciplinary investigation is currently underway. We intend to determine the age of three Darwin Glasses with the 40Ar-39Ar technique at the University of Bern. We thus hope to obtain a precise age which will permit or deny verification of multiple impacts large distances apart. New samples, taken from the country rock of the proposed Darwin Crater site, are currently being studied for microscopic impact features. Mathematical calculations will be performed to test possible impact scenarios for the likelihood of contemporaneity of multiple impact events in the Australasian strewn field area. References: [1] Gentner W. et al. (1973) EPSL, 20, 204-210. [2] Kunz J. et al. (1995) LPS XXVI, 809.

The chemical durability of tektites - A laboratory study and correlation with long-term corrosion behavior

NASA Technical Reports Server (NTRS)

Barkatt, A.; Boulos, M. S.; Barkatt, A.; Sousanpour, W.; Boroomand, M. A.; Macedo, P. B.; Okeefe, J. A.

1984-01-01

Leach tests carried out on tektite specimens (indochinites and australites) under high-dilution conditions show a common behavior characterized by low leach rates (0.00018 g/sq m per d, or 7.2 x 10 to the -12th m/d at 23 C) and an activation energy of (79,600 + or - 700 J/mol). The extent of selective leaching is very small, of the order of 10 to the -8th m. Extrapolation of test results over the lifetime of the tektites gives an excellent agreement with field observations on the extent of corrosion, and this is an important step in establishing the validity of laboratory tests as a basis for the development of models and predictions concerning long-term durabilities at least in the limiting case of high dilution or rapid flow. The results are also shown to be in agreement with various previous observations on the corrosion resistance of tektites. The chemical durability of tektites is observed to be consistent with their composition, highlighting requirements of high corrosion resistance in glasses; these requirements include a silica content in excess of 67 mol percent, an extremely low water content, and an alkali content which is low both absolutely and relative to the di- and poly-valent metal oxide levels. It is shown that artificial glasses which fulfil these criteria are no less corrosion-resistant than the corresponding natural glasses. These conclusions have bearing on the development, as well as on the evaluation, of glasses intended for very long service, such as radioactive waste vitrification media.

The Origin of Tektites

NASA Technical Reports Server (NTRS)

OKeefe, J. A.

1960-01-01

Tektites are probably extraterrestrial, rather than the result of heating some terrestrial materials, because they are a chemically homogeneous group with definite peculiarities (high silica, excess of alkaline earths over alkalis, excess of potash over soda, absence of water), and because some of them (the australites) appear to have undergone ablation in flight through the atmosphere. Since comparatively slow heating is required to explain the liquefaction of the tektite material, it is suggested that the tektites arrived along orbits which were nearly parallel to the surface of the earth, and which resulted from the decay of the orbit of a natural satellite. The great meteor procession of February 9, 1913, is an example of such an object. Comparison with the reentry phenomena of the artificial satellite 1957 Beta suggests that the 1913 shower consisted of a single large stone weighing about 400 kilograms, and a few dozen smaller bodies weighing about 40 grams each, formed by ablation from the larger body. It is shown that under the observed conditions considerable liquid flow would be expected in the stone, which would be heated to about 2100 K. Objects falling from such a shower near the perigee point of the orbit would have a considerable distribution along the orbit as a result of slight variations in height or drag coefficient. The distribution in longitude would be made wider by the turning of the earth under the orbit during the time of fall. The ultimate source of the body which produces a tektite shower is probably the moon, which appears, by virtue of its polarization and the phase distribution of the returned light, to contain high-silica materials. It is suggested that the Igast object alleged to have fallen in 1855 is in fact genuine and represents an unmelted portion of the lunar crust.

Tektite origin by hypervelocity asteroidal or cometary impact: The quest for the source craters

NASA Technical Reports Server (NTRS)

Koeberl, Christian

1992-01-01

Tektites are natural glasses that are chemically homogeneous, often spherically symmetrical objects several centimeters in size, and occur in four known strewn fields on the surface of the Earth: the North American, moldavite (or Central European), Ivory Coast, and Australasian strewn fields. Tektites found within such strewn fields are related to each other with respect to their petrological, physical, and chemical properties as well as their age. A theory of tektite origin needs to explain the similarity of tektites in respect to age and certain aspects of isotopic and chemical composition within one strewn field, as well as the variety of tektite materials present in each strewn field. In addition to tektites on land, microtektites (which are generally less than 1 mm in diameter) have been found in deep-sea cores. Tektites are classified into three groups: (1) normal or splash-form tektites, (2) aerodynamically shaped tektites, and (3) Muong Nong-type tektites (sometimes also called layered tektites). The aerodynamic ablation results from partial remelting of glass during atmospheric passage after it was ejected outside the terrestrial atmosphere and quenched from a hot liquid. Aerodynamically shaped tektites are known mainly from the Australasian strewn field where they occur as flanged-button australites. The shapes of splash-form tektites (spheres, droplets, teardrops, dumbbells, etc., or fragments thereof) are the result of the solidification of rotating liquids in the air or vacuum. Mainly due to chemical studies, it is now commonly accepted that tektites are the product of melting and quenching of terrestrial rocks during hypervelocity impact on the Earth. The chemistry of tektites is in many respects identical to the composition of upper crustal material.

New data on selected Ivory Coast tektites

USGS Publications Warehouse

Cuttitta, F.; Carron, M.K.; Annell, C.S.

1972-01-01

Fourteen Ivory Coast tektites exhibit a range of bulk indices of refraction of 1.5156 to 1.5217 ?? 0.0004 and of bulk specific gravities of 2.428 to 2.502 ??0.005. Seven of these Ivory Coast (IVC) tektites were analyzed for major and minor element content. Compared to tektites from other strewn fields, their SiO2 content is low (67.2-69.1 %), A12O3 relatively high (15.8-16.8 %), and total iron relatively high but with a more restricted range (6.3-6.8 % as FeO). Their lime content is low (0.71-1.35%) compared to Australasian tektites but their MgO CaO ratio (about 3.1) is unusually high. All other tektite groups have Na2O K2O ratios less than unity, but the Na2O K2O ratio of the IVC tektites is slightly greater than unity. Their K Rb ratios range from 200 to 256 and average 227, which is higher than those determined for Australasian tektites, but similar to some obtained for moldavites. The Li content (41-48 ppm) is about the same as that of the Australasian tektites, but the Cs and Rb are lower, being 1.9 to 2.9 and 57 to 86 ppm, respectively. The IVC tektites are high in Cr (260-375 ppm), Co (19-25 ppm) and Ni (101-167 ppm), and particularly in Pb (<10-18 ppm), Cu (13-21 ppm) and Ga (14-23 ppm). The high Cr Ni ratios of the IVC tektites (range 2-3.6) are similar to those found for australites, philippinites and thailandites, but not the javanites and indochinites. Evaluation of these and other reported data show that compositional similarities between the IVC tektites and green or black Bosumtwi Crater glasses strongly support the hypothesis of a common impact origin-i.e. the Bosumtwi Crater site. Comparison of the IVC tektite composition with those of returned lunar materials (gabbros, basalts, breccia and soils) do not support a lunar origin for the Ivory Coast tektites. ?? 1972.

Age of the Australasian Tektite Strewn Field

NASA Astrophysics Data System (ADS)

Izokh, E. P.

1993-07-01

As Fig. 1 shows, the widespread belief that the age of the Australasian tektite strewn field (AATSF) is ~0.7 m.y. appeared to be conventional. Tektites of different fission-track ages were found within the AATSF: 0.83 m.y. [1], 3.54-4.25 m.y. [2], and ~11 m.y. [3]. The first systematic investigation of the tektites, which were collected from a single stratigraphic layer in Vietnam, revealed three statistically discrete tektite age groups: 0.4, 0.6, and 0.8 m.y. [4]. Similar tektites 0.75 m.y. and 1.1 m.y. in age are typical of the Zhamanshin impact crater, which represents an eminent part of the AATSF [5]. Fig. 1, which appears here in the hard copy, shows radiogenic dating: 1-2: AATSF; 3-4: Zhamanshin; 1,3: data with known annealing correction. Compiled after Zahringer, 1963; Fleischer and Price, 1964; Gentner et al., 1969; McDougal and Lovering, 1969; Fleischer et al., 1969; Storzer and Wagner, 1979, 1980; Watanabe et al., 1985; Virk, 1985; Shukolukov et al., 1986; Kashkarov et al, 1986, 1987; Kolesnikov et al., 1987; Storzer and Muller-Sonhius, 1986; Arakelyants et al., 1988; etc. The very young geological age of the AATSF was established in Australia, and was confirmed by the author in Vietnam and in the Zhamanshin impact crater. This well-known tektite age paradox strongly supports an extraterrestrial origin of tektites. The paradox is fatal to the currently dominating Earth- impact theory of tektite origin, and we are not surprised that there are no continued attempts to either silence or disavow its significance. As a matter of fact, the formation of the gigantic AATSF can be considered as the main reason for the abrupt catastrophic climatic global changes and mass extinction of species on the Pleistocene/Holocene boundary 10,000 years ago [5,6]. The age-paradox scope dictates that tektites have been periodically formed and accumulated somewhere on an as-yet-unknown planetary body and then delivered to the Earth. The extraterrestrial volcanic eruptions seem to be the most appropriate process of the tektite formation and launching [7]. The frequent shift of the K-Ar ages relative to the fission-track ages of tektites can be explained by the presence of an extra argon inherited from some older crystalline inclusions foreign to the tektite glass. These inclusions are most common to the Muong Nong-type layered tektites and to flanges of the button-shape australites, and can be considered as an extraterrestrial environmental dust peppering. References: [1] Storzer and Wagner (1980) Meteoritics, 15, 372. [2] Fleischer et al. (1969) EPSL, 7, 51-52. [3] Storzer and Muller-Sonhius (1986) Meteoritics, 21, 518-519. [4] Kashkarov et al. (1986) Meteoritika, 45, 105-170. [5] Izokh (1991) Soviet Geol. and Geophys., 32, 1-10. [6] Tollman and Tollmann (1992) Mitt. Osterr. Geol. Ges., 84. [7] Izokh and Le duc An (1983) Meteoritika, 42, 158-169.