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Sample records for alba patera mars

  1. Alba Patera

    NASA Technical Reports Server (NTRS)

    1997-01-01

    A color image of the Alba Patera region of Mars; north toward top. The scene shows a central circular depression surrounded by splays of fractures, named Alba Fossae (west of Alba Patera) and Tantalus Fossae (east of Alba Patera). A patera (Latin for shallow dish or saucer) is a volcano of broad areal extent with little vertical relief; a fossa is a linear depression.

    This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 30 degrees N. to 50 degrees N. and from longitude 95 degrees to 125 degrees; Lambert projection.

    Alba Patera has a 100-km-diameter caldera at its center surrounded by a fracture ring. In total, the approximately 1,200- km-diameter Alba Patera far exceeds any other known volcano in areal extent; it covers eight times the area of Olympus Mons (the highest volcano in the Solar System) but reaches only about 6 km in height. The patera lies directly north of the Tharsis bulge, which encompasses the most intensely and most recently active volcanic region of the planet. The fossae of the Alba area are fault-bound graben that can be traced south through the Tharsis bulge and therefore likely formed by upwarping of the Tharsis bulge as well as the coeval upwelling of Alba Pateria magma.

  2. Polygenic eruptions on Alba Patera, Mars

    NASA Technical Reports Server (NTRS)

    Mouginis-Mark, P. J.; Wilson, L.; Zimbelman, J. R.

    1988-01-01

    A new model for the evolution of the martian volcano Alba Patera is constructed. Numerous digitate channel networks on the flanks of the volcano are interpreted to be carved by sapping due to the release of nonjuvenile water from unconsolidated flank deposits. The particle size of these deposits is estimated to be 3-10 microns, which, together with theoretical modelling of the disperison of explosively derived volcanic materials, leads to the conclusion that the flank deposits on Alba Patera are low-relief pyroclastic flows. The recognition of numerous late-stage summit and subterminal lava flows thus makes Alba Patera a unique martian volcano that is transitional between the older pyroclastic-dominated highland paterae and the more recent effusive central-vent volcanoes such as the Tharsis Montes.

  3. Geomorphology and stratigraphy of Alba Patera, Mars

    NASA Technical Reports Server (NTRS)

    Schneeberger, Dale M.; Pieri, David C.

    1991-01-01

    Geomorphic and stratigraphic analysis of Alba Patera suggests a volcanic construct built by lavas with rheologic properties similar to basalts. A series of evolving eruptive styles is suggested by changes in morphology and inferred progressive reductions in flow volume with higher stratigraphic position. Alba Patera's volcanic history has been summarized into four main phases. The first is characterized by extensive flood like flows presumably erupted from fissures associated with the initial intrusion of magma into the region. The second phase is associated with the emplacement of pyroclastic rock, a more speculative interpretation. The third phase produced the voluminous tabular, crested, and undifferentiated flows, probably from a more centralized vent source. The fourth and last phase is marked the effusion of levee like flows and the collapse of the summit calderas and final graben formation.

  4. Relative ages of lava flows at Alba Patera, Mars

    NASA Technical Reports Server (NTRS)

    Schneeberger, Dale M.; Pieri, David C.

    1987-01-01

    Many large lava flows on the flanks of Alba Patera are astonishing in their volume and length. As a suite, these flows suggest tremendously voluminous and sustained eruptions, and provide dimensional boundary conditions typically a factor of 100 larger than terrestrial flows. One of the most striking features associated with Alba Patera is the large, radially oriented lava flows that exhibit a variety of flow morphologies. These include sheet flows, tube fed and tube channel flows, and undifferentiated flows. Three groups of flows were studied; flows on the northwest flank, southeast flank, and the intracaldera region. The lava flows discussed probably were erupted as a group during the same major volcanic episode as suggested by the data presented. Absolute ages are poorly constrained for both the individual flows and shield, due in part to disagreement as to which absolute age curve is representative for Mars. A relative age sequence is implied but lacks precision due to the closeness of the size frequency curves.

  5. Alba Patera

    NASA Technical Reports Server (NTRS)

    2002-01-01

    (Released 22 April 2002) The Science This image, centered near 46.5 N and 119.3 W (240.7 E), is on the northwestern flank of a large, broad shield volcano called Alba Patera. This region of Mars has a number of unique valley features that at first glance look dendritic much in the same pattern that rivers and tributaries form on Earth. A closer look reveals that the valleys are quite discontinuous and must form through a different process than surface runoff of liquid water that is common on Earth. A number of processes might have taken place at some point in the Martian past to form these features. Some of the broad valley features bear some resemblance to karst topography, where material is removed underground by melting or dissolving in groundwater causing the collapse of the surface above it. The long narrow valleys resemble surfaces where groundwater sapping has occurred. Sapping happens when groundwater reaches the surface and causes headward erosion, forming long valleys with fewer tributaries than is seen with valleys formed by surface water runoff. The volcano itself might have been a source of heat and energy, which played a role in producing surfaces that indicate an active groundwater system. The Story Fluid, oozing lava poured somewhat lazily over this area long ago. It happened perhaps thousands of times, over hundreds of thousands of Martian years, creating the nearly smooth, plaster-of-Paris-looking terrain seen today. (Small craters also dent the area, though they may deceive you and look like raised bumps instead. That's just a trick of the eye and the lighting - tilt your head to your left shoulder, and you should see the craters pit the surface as expected.) The lava flows came from a Martian 'shield' volcano named Alba Patera. Shield volcanoes get their name from their appearance: from above, they look like large battle shields lying face up to the sky as if a giant, geological warrior had lain them down. Perhaps one did if you think of a

  6. Tectonic histories between Alba Patera and Syria Planum, Mars

    USGS Publications Warehouse

    Anderson, R.C.; Dohm, J.M.; Haldemann, A.F.C.; Hare, T.M.; Baker, V.R.

    2004-01-01

    Syria Planum and Alba Patera are two of the most prominent features of magmatic-driven activity identified for the Tharsis region and perhaps for all of Mars. In this study, we have performed a Geographic Information System-based comparative investigation of their tectonic histories using published geologic map information and Mars Orbiter Laser Altimetry (MOLA) data. Our primary objective is to assess their evolutional histories by focusing on their extent of deformation in space and time through stratigraphic, paleotectonic, topographic, and geomorphologic analyses. Though there are similarities among the two prominent features, there are several distinct differences, including timing deformational extent, and tectonic intensity of formation. Whereas Alba Patera displays a major pulse of activity during the Late Hesperian/Early Amazonian, Syria Planum is a long-lived center that displays a more uniform distribution of simple graben densities ranging from the Noachian to the Amazonian, many of which occur at greater distances away from the primary center of activity. The histories of the two features presented here are representative of the complex, long-lived evolutional history of Tharsis. ?? 2004 Elsevier Inc. All rights reserved.

  7. Estimates of lava eruption rates at Alba Patera, Mars

    NASA Astrophysics Data System (ADS)

    Baloga, S. M.; Pieri, D. C.

    1985-04-01

    The Martian volcanic complex Alba Patera exhibits a suite of well-defined, long and relatively narrow lava flows qualitatively resembling those found in Hawaii. Even without any information on the duration of the Martian flows, eruption rates (total volume discharge/duration of the extrusion) estimates are implied by the physical dimensions of the flows and the likely conjecture that Stephan-Boltzmann radiation is the dominating thermal loss mechanism. The ten flows in this analysis emanate radially from the central vent and were recently measured in length, plan areas, and average thicknesses by shadow measurement techniques. The dimensions of interest are shown. Although perhaps morphologically congruent to certain Hawaiian flows, the dramatically expanded physical dimensions of the Martian flows argues for some markedly distinct differences in lava flow composition for eruption characteristics.

  8. Volcanic styles at Alba Patera, Mars: Implications of lava flow morphology to the volcanic history

    NASA Technical Reports Server (NTRS)

    Schneeberger, D. M.; Pieri, D. C.

    1988-01-01

    Alba Patera presents styles of volcanism that are unique to Mars. Its very low profile, large areal extent, unusually long and voluminous lava flows, and circumferential graben make it among Mars' most interesting volcanic features. Clues to Alba's volcanic history are preserved in its morphology and stratigraphy. Understanding the relationship of lava flow morphology to emplacement processes should enable estimates of viscosity, effusion rate, and gross composition to be made. Lava flows, with dimensions considered enormous by terrestrial standards, account for a major portion of the exposed surface of Alba Patera. These flows exhibit a range of morphologies. While most previous works have focused on the planimetric characteristics, attention was drawn to the important morphological attributes, paying particular attention to what the features suggest about the emplacement process.

  9. Alba Patera Windstreaks

    NASA Technical Reports Server (NTRS)

    2005-01-01

    [figure removed for brevity, see original site]

    Windstreaks are features caused by the interaction of wind and topographic landforms. The raised rims and bowls of impact craters causes a complex interaction such that the wind vortex in the lee of the crater can both scour away the surface dust and deposit it back in the center of the lee. If you look closely, you will see evidence of this in a darker 'rim' enclosing a brighter interior.

    These windstreaks are located northeast of Olympus Mons and southwest of Alba Patera. The lava flows the windstreaks occur on most likely originated from Alba Patera.

    Image information: VIS instrument. Latitude 31.3, Longitude 235.1 East (124.9 West). 36 meter/pixel resolution.

    Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.

    NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

  10. Alba Patera Collapse Pits

    NASA Technical Reports Server (NTRS)

    2004-01-01

    [figure removed for brevity, see original site]

    We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form.

    These collapse pits are found within graben surrounding Alba Patera. Alba Patera is an old volcano that has subsided after it's magma chamber was evacuated.

    Image information: VIS instrument. Latitude 43.1, Longitude 259.4 East (100.6 West). 19 meter/pixel resolution.

    Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.

    NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA

  11. Alba Patera Collapse Pits

    NASA Technical Reports Server (NTRS)

    2004-01-01

    [figure removed for brevity, see original site]

    We will be looking at collapse pits for the next two weeks. Collapse pits on Mars are formed in several ways. In volcanic areas, channelized lava flows can form roofs which insulate the flowing lava. These features are termed lava tubes on Earth and are common features in basaltic flows. After the lava has drained, parts of the roof of the tube will collapse under its own weight. These collapse pits will only be as deep as the bottom of the original lava tube. Another type of collapse feature associated with volcanic areas arises when very large eruptions completely evacuate the magma chamber beneath the volcano. The weight of the volcano will cause the entire edifice to subside into the void space below it. Structural features including fractures and graben will form during the subsidence. Many times collapse pits will form within the graben. In addition to volcanic collapse pits, Mars has many collapse pits formed when volatiles (such as subsurface ice) are released from the surface layers. As the volatiles leave, the weight of the surrounding rock causes collapse pits to form.

    This image of the Alba Patera region has both lava tube collapse pits (running generally east/west) and subsidence related collapse within structural grabens.

    Image information: IR instrument. Latitude 26.9, Longitude 256.5 East (103.5 West). 100 meter/pixel resolution.

    Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.

    NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA

  12. Geomorphic signatures of glacial activity in the Alba Patera volcanic province: Implications for recent frost accumulation on Mars

    NASA Astrophysics Data System (ADS)

    Sinha, Rishitosh K.; Murty, Sripada V. S.

    2013-08-01

    landforms lying within impact craters on Mars have led to the identification of two mechanisms for their formation: (1) intermittent deposition of atmospherically emplaced snow/ice during past spin-axis/orbital conditions and (2) flow of debris-covered ice-rich deposits. The maximum presence of the young ice/snow-rich features (thermal contraction crack polygons, gullies, arcuate ridges, and lobate debris tongues) was observed on the pole-facing slope, indicating that this slope was the preferred site for ice/snow accumulation (during the last 10 Ma). In this study, we investigated 30 craters lying in the Alba Patera volcanic province in the latitudinal bands between 45°N and 32.4°N. Morphological comparison of the younger ice/snow-rich features in these craters led us to conclude that glacial/periglacial features in Alba Patera are mainly present within pole-facing slopes of craters lying within 45°N-39°N. The craters lying within 40.2°N-40°N did not show any glacial/periglacial features. We suggest that the formation of these young ice/snow-rich features follows the same orientation trends as those of other older (>10 Ma) glacial features (debris-covered ice/snow-rich large deposits at the base of the crater wall) in the region. The present work has revealed that the onset of physical processes that result in the formation of glacial/periglacial landforms is also dependent on the changes in elevation ranges of the investigated craters in Alba Patera. Our results confirm past inferences for accumulation of ice/snow on Mars and suggest that the period of ice/snow accumulation activity in Alba Patera occurred throughout the Amazonian and lasted until the recent past, i.e., 2.1-0.4 Ma.

  13. Valleys on Northwest Flank of Alba Patera Volcano

    NASA Technical Reports Server (NTRS)

    1999-01-01

    In 1972, Mariner 9 images revealed a variety of branched and networked valleys on Alba Patera, a volcano in northern Tharsis. Since then, the question has always been, 'what made these valleys, water or lava?' Because the Alba Patera volcano was considered to be a relatively young feature on Mars, it seemed that if waterways involved in the formation of the valleys, then it would imply that liquid water flowed on this part of Mars at a relatively recent time in the planet's history. Thus, it was hoped that Mars Global Surveyor (MGS), with its super-high resolution Mars Orbiter Camera (MOC), would help answer this key question about evidence for past water on the red planet.

    However, when MOC peered down upon these valleys it became clear that the camera might not help answer the question of their origin. As the picture above shows, these valleys--which trend from lower right to upper left in the picture--are old and have been cut by younger faults that created graben--e.g., the wide, straight valley running diagonally from upper right to lower left. Worse, the close-up views revealed that the valleys are covered up by a lumpy-textured material that also partly fills nearby impact craters. The origin of the textured material is unknown but might result from years and years of wind erosion of surface 'soil' or volcanic ash. However it formed, this covering obscures so much of the details of the valleys that high resolution pictures are unlikely to solve this mystery.

    The picture above covers an area approximately 8 kilometers (5 miles) wide by 15 kilometers (9 miles) high. Illumination is from the right. The picture was acquired in August 1998 during the MGS Science Phasing Orbits imaging campaign, and was presented at the 30th Lunar and Planetary Science Conference in Houston, Texas, March 1999.

    Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the

  14. Fractal geometry of some Martian lava flow margins: Alba Patera

    NASA Technical Reports Server (NTRS)

    Kauhanen, K.

    1993-01-01

    Fractal dimension for a few lava flow margins on the gently sloping flanks of Alba Patera were measured using the structured walk method. Fractal behavior was observed at scales ranging from 20 to 100 pixels. The upper limit of the linear part of log(margin length) vs. log(scale) profile correlated well to the margin length. The lower limit depended on resolution and flow properties.

  15. Mapping Tyrrhena Patera and Hesperia Planum, Mars

    NASA Technical Reports Server (NTRS)

    Crown, David A.

    2009-01-01

    Hesperia Planum, characterized by a high concentration of mare-type wrinkle ridges and ridge rings [1-4], encompasses > 2 million sq km in the southern highlands of Mars (Fig. 1). The most common interpretation is that the plains were emplaced as "flood" lavas with total thicknesses of <3 km [4-10]. The wrinkle ridges on its surface make Hesperia Planum the type locale for "Hesperian-aged ridged plains" on Mars [e.g., 9], and recent investigations reveal that wrinkle-ridge formation occurred in more than one episode [4]. Hesperia Planum?s stratigraphic position and crater-retention age [e.g., 9, 11-12] define the base of the Hesperian System. However, results of geologic mapping reveal that the whole of Hesperia Planum is unlikely to be composed of the same materials, emplaced at the same geologic time. To unravel these complexities, we are generating a 1:1.5M-scale geologic map of Hesperia Planum and its surroundings (Fig. 1). We have identified 4 distinct plains units within Hesperia Planum and are attempting to determine the nature and relative ages of these materials (Fig. 2) [13, 14]. The volcano Tyrrhena Patera (22degS, 104degE) is located within Hesperia Planum. Its products are both embayed by, and superpose, Hesperia Planum materials [15, 16]. We were previously funded to generate a 1:1 million scale map of Mars Transverse Mercator (MTM) quadrangles -15257 and -20257, which include the Tyrrhena Patera materials north and west of the Tyrrhena Patera summit. The goal for these maps was to constrain the nature and extent of the Tyrrhena Patera deposits, and to determine the relationship between Tyrrhena Patera materials, Hesperia Planum, and the adjacent highlands [16].

  16. Candidate Mars Surveyor Landing Sites Near Apollinaris Patera

    NASA Astrophysics Data System (ADS)

    Gulick, Virginia C.

    1999-06-01

    Regions near Apollinaris Patera are proposed for consideration as Mars Surveyor landing sites. Gulick (1998) proposed this region at the First Mars Surveyor Landing Site workshop; Bulmer and Gregg (1998) provided additional support. Apollinaris Patera is situated on the highlands/lowlands boundary at 8.5S, 186W. The volcano itself has been mapped as Hesperian in age. The regions surrounding Apollinaris show evidence for volcanism, volcano-ice interactions, and erosion by water. Numerous valleys modified by fluvial processes dissect a large fan structure emanating from the southern flank of the volcano. Sapping valleys have formed along the southern terminus of the fan structure. Regions near Apollinaris Patera provide a unique opportunity to sample outcrop lithologies ranging from highland Noachian basement rocks, to Hesperian aged lava flows, channel and flood plain materials, to Amazonian volcanic, ash and channel deposits.

  17. The Bulk Density of the Tyrrhena Patera Highland Volcano, Mars

    NASA Astrophysics Data System (ADS)

    Grott, M.; Wieczorek, M. A.

    2011-12-01

    Tyrrhena Patera is a low-relief, central-vent volcano located in the southern highlands of Mars, northeast of the Hellas impact basin. The main edifice contains few primary lave flow features and the flanks of the volcano are heavily eroded, indicating that they are composed of friable material which could have been formed by pyroclastic flows. The volcano itself was emplaced in the Noachian, but was subsequently modified during the Hesperian period, with episodes of resurfacing - probably driven by erosion - stretching well into the Amazonian period. Resurfacing of the caldera rille floor and upper shield probably mark the cessation of volcanic activity at Tyrrhena Patera around 800 Ma ago, and the geological evidence suggests that activity at Tyrrhena Patera transitioned from dominantly explosive to dominantly effusive eruptions. In summary, Tyrrhena Patera is generally thought to be predominantly composed of multi-layered, compacted ignimbrite deposits. The Tyrrhena Patera volcano is associated with a well localized positive free-air gravity anomaly and a good correlation exists with the features topography. We have used the latest gravity field model for Mars expanded up to degree and order 110 to model the localized admittance spectrum at Tyrrhena Patera considering surface as well as subsurface loading. We use a spherical cap localization window with a cap diameter of 7 degrees and a spherical harmonic bandwidth of 37. Ignoring the lowest degree terms that may be influenced by the Tharsis signal, we analyze the localized admittance in the degree range 42 to 57. The observed admittance is then compared to a forward model which is localized in the same manner as the data. In this way, we have quantified the range of admissible load densities as well as the admissible magnitude of a potentially present subsurface load. Modelling suggests that load densities need to be between 3290 and 3450 kg/m3 if no subsurface loads are present. If subsurface loads in the form

  18. Geologic Map of the MTM -30262 and -30267 Quadrangles, Hadriaca Patera Region of Mars

    USGS Publications Warehouse

    Crown, David A.; Greeley, Ronald

    2007-01-01

    Introduction Mars Transverse Mercator (MTM) -30262 and -30267 quadrangles cover the summit region and east margin of Hadriaca Patera, one of the Martian volcanoes designated highland paterae. MTM -30262 quadrangle includes volcanic deposits from Hadriaca Patera and Tyrrhena Patera (summit northeast of map area) and floor deposits associated with the Dao and Niger Valles canyon systems (south of map area). MTM -30267 quadrangle is centered on the caldera of Hadriaca Patera. The highland paterae are among the oldest, central-vent volcanoes on Mars and exhibit evidence for explosive eruptions, which make a detailed study of their geology an important component in understanding the evolution of Martian volcanism. Photogeologic mapping at 1:500,000-scale from analysis of Viking Orbiter images complements volcanological studies of Hadriaca Patera, geologic investigations of the other highland paterae, and an analysis of the styles and evolution of volcanic activity east of Hellas Planitia in the ancient, cratered highlands of Mars. This photogeologic study is an extension of regional geologic mapping east of Hellas Planitia. The Martian highland paterae are low-relief, areally extensive volcanoes exhibiting central calderas and radial channels and ridges. Four of these volcanoes, Hadriaca, Tyrrhena, Amphitrites, and Peneus Paterae, are located in the ancient cratered terrains surrounding Hellas Planitia and are thought to be located on inferred impact basin rings or related fractures. Based on analyses of Mariner 9 images, Potter (1976), Peterson (1977), and King (1978) suggested that the highland paterae were shield volcanoes formed by eruptions of fluid lavas. Later studies noted morphologic similarities between the paterae and terrestrial ash shields and the lack of primary lava flow features on the flanks of the volcanoes. The degraded appearances of Hadriaca and Tyrrhena Paterae and the apparently easily eroded materials composing their low, broad shields further

  19. Volcanic geology of Hadriaca Patera and the eastern Hellas region of Mars

    NASA Astrophysics Data System (ADS)

    Crown, D. A.; Greeley, R.

    1993-02-01

    A detailed examination of the geomorphology of Hadriaca Patera, a low-relief volcano in the southern highlands of Mars northeast of the Hellas basin, is presented, and the surrounding eastern Hellas region is considered in order to assess whether the volcanic geology of Hadriaca Patera is consistent with previous characterizations and highland paterae. The morphologic characteristics of the channels suggest erosion by groundwater sapping and surface runoff. The erosional morphology of the volcano, the lack of lava flow features, and the friable nature of the flank materials indicate that Hadriaca Patera consists predominantly of pyroclastic deposits. From the predominance of hydrovolcanic eruptions in the development of Hadriaca and Tyrrhena patera, it is inferred that the transition in volcanic eruption style can be attributed to a volatile depletion of the crust, whereas magmatic eruptions at the paterae would be indicative of temporal changes in Martian magmas.

  20. Amphitrites Patera

    NASA Technical Reports Server (NTRS)

    1997-01-01

    A color image of the Amphitrites Patera region of Mars; north toward top. The scene shows several indistinct ring structures and radial ridges of an old volcano named Amphitrites Patera. A patera (Latin for shallow dish or saucer) is a volcano of broad areal extent with little vertical relief.

    This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 55 degrees S. to 62 degrees S. and from longitude 292 degrees to 311 degrees; Lambert projection.

    Amphitrites Patera is a 138-km-diameter feature on the south rim of Hellas impact basin and is one of many indistinct ring structures in the area. The location of the paterae in this area of Hellas indicates that their source magma may have been influenced by the transition fractures of the basin. The radial ridges of Amphitrites extend for about 400 km north into the Hellas basin.

  1. The Martian highland paterae: Evidence for explosive volcanism on Mars

    NASA Technical Reports Server (NTRS)

    Crown, David A.; Greeley, Ronald

    1988-01-01

    The Martian surface exhibits numerous volcanic landforms displaying great diversity in size, age, and morphology. Most research regarding Martian volcanology has centered around effusive basaltic volcanism, including analyses of individual lava flows, extensive lava plains, and large shield volcanoes. These studies were hindered by a lack of definitive morphologic criteria for the remote identification of ash deposits. Knowledge of the abundances, ages, and geologic settings of explosive volcanic deposits on Mars is essential to a comprehensive understanding of the evolution of the Martian surface, with implications for the evolution of the lithosphere and atmosphere as well as the histories of specific volcanic centers and provinces.

  2. Deep Basalt Aquifers in Orcus Patera, Elysium Basin Mars: Perspectives for Exobiology Exploration

    NASA Technical Reports Server (NTRS)

    Grin, E. A.; Cabrol, N. A.

    1998-01-01

    Direct indicators of shorelines, spillways, and terraces allowed to determine the extent of the Elysium Paleolake between the contour-lines 1000 and 500 m below the Martian datum. The Elysium Paleolake is bordered north by Orcus Patera (14N/181W), which lies west of the Tartarus Montes and Tartarus Colles. The Orcus Patera displays an ellipse-shaped collapsed caldera of 360-km long and 100-km wide. Viking topographic data show that the bottom of the caldera is located at 2500 below the Martian datum, and surrounded by a steep-walled ram art which crest is located at about 0 m elevation. Considering the localization of Orcus Patera in the Elysium paleolake, its altimetry, and the magmatic origin of this caldera, we propose the existence of a paleolake in Orcus Patera generated (a) by juvenile water from magma during the Noachian period, and (b) by intermittent influx of the Elysium Basin from Hesperian to Amazonian. Results are encouraging to consider this site as a potential high-energy source environment for microbial communities. are circumscribed by a 50-km wide lava field mapped as Noachian material. The structure of Orcus Patera represents the record of material erupted from a magmatic reservoir. The caldera is enclosed by steep inner walls (25% measured from topographic data), values which could be in agreement with the presence of a deep magmatic reservoir, as suggested by the typology of Crumpler et.al. The depth of the caldera might be due to the collapse of the magma reservoir, and the release of gases accompanying the magma thermal evolution. Origins of water for the paleolake(s): The water that generated a paleolake in Orcus Patera may have come from two origins: (1) Juvenile water: Plescia and Crips estimated a magma H20 content by weight between 0.5% and 1.5% using for the first value a comparison with terrestrial basalt, and for the second values from a Martian meteorite. The amount of H20 can be estimated by the volume of erupted lava, and the lava

  3. Tyrrhena Patera

    NASA Technical Reports Server (NTRS)

    1997-01-01

    A color image of the Tyrrhena Patera Region of Mars; north toward top. The scene shows a central circular depression surrounded by circular fractures and highly dissected horizontal sheets. A patera (Latin for shallow dish or saucer) is a volcano of broad areal extent with little vertical relief. This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 17 degrees S. to 25 degrees S. and from longitude 250 degrees to 260 degrees; Mercator projection. Tyrrhena Patera has a 12-km-diameter caldera at its center surrounded by a 45-km-diameter fracture ring. Around the fracture ring, the terrain is highly eroded forming ragged outward-facing cliffs, as though successive flat-lying layers had been eroded back. Cut into the sequence are several flat-floored channels that extend outward as far as 200 km from the center of the volcano. The structure may be composed of highly erodible ash layers and the channels may be fluvial, with the release of water being triggered by volcanic activity (Carr, 1981, The surface of Mars, Yale Univ. Press, New Haven, 232 p.).

  4. Nature of Hesperian Resurfacing in the Scandia-North Polar Region of Mars

    NASA Astrophysics Data System (ADS)

    Tanaka, K. L.; Rodriguez, J. A. P.; Fortezzo, C. M.; Hayward, R. K.; Skinner, J. A.

    2010-03-01

    Formational hypotheses based on preliminary observations and first-year mapping results of the Scandia-North Polar Region of Mars. The map area includes the Scandia Cavi, Scandia Tholi, Scandia Colles, northern Alba Patera, and Vastitas Borealis.

  5. Hadriaca Patera

    NASA Technical Reports Server (NTRS)

    1997-01-01

    A color image of Hadriaca Patera on the northeast rim of Hellas basin of Mars; north toward top. The scene shows a central circular depression surrounded by low radial ridges and, at the bottom of the image, the channel of Dao Vallis. A patera (Latin for shallow dish or saucer) is a volcano of broad areal extent with little vertical relief.

    This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 27 degrees S. to 37 degrees S. and from longitude 263 degrees to 273 degrees; Mercator projection.

    Hadriaca Patera is less than 2 km high, has a 60-km-diameter caldera at its center, and is surrounded by a 300-km-wide ring of low ridges. The radial ridges may be lava flows with lava channels at their crests. South of Hadriaca, Dao Vallis begins at a steep-walled depression 40 km across but forms a much shallower channel that extends 800 km southwest into the floor of the Hellas basin. The channel is very likely fluvial in origin, with the release of water being triggered by volcanic activity.

  6. Apollinaris Patera

    NASA Technical Reports Server (NTRS)

    1997-01-01

    A color image of the Apollinaris Patera Region of Mars; north toward top. The scene shows the 80-km-wide central caldera of Apollinaris, a plume of young flows extending south down the flank of the volcano, a cliff and chaotic terrain west of the volcano, and the surrounding younger deposits of the Medusae Fossae Formation (north and east). A patera (Latin for shallow dish or saucer) is a volcano of broad areal extent with little vertical relief. This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 12 degrees S. to 6 degrees S. and from longitude 182 degrees to 189 degrees; Mercator projection. Apollinaris Patera is an isolated volcano (about 400 km across) lying on the Martian highlands just north of Gusev impact crater and the termination of Ma'adim Vallis. After the main edifice was built, eruption continued on the volcano's southern flank to form a broad ridge overlapping the original shield. Breakdown of ice-rich materials formed chaos on its western edge. Finally the friable materials (possible ash?) of the Medusae Fossae Fm were deposited.

  7. Areal Distribution of Potential Felsic Material in Nili Patera at Syrtis Major, Mars

    NASA Astrophysics Data System (ADS)

    Eggers, G. L.; Wray, J. J.; Dufek, J.

    2015-12-01

    For decades, studies of the exposed igneous Martian crust via remote sensing and landed observation have concluded that it is predominantly basaltic. However, new analyses of meteorites and mission data indicate a wider range of primary rock composition. Nili Patera in the Syrtis Major region provides one of the best exposures of evolved compositions. Recently, Wray et al. (2013) identified a new unit in the caldera with very high feldspar abundance but unusually low mafic abundance and interpreted it as a felsic unit (as opposed to spectrally similar anorthosite) based on its proximity to a dacite unit. We investigate the summit calderas of Syrtis Major by defining and mapping distinct compositional units using mineralogies inferred from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument on the Mars Reconnaissance Orbiter (MRO). The study focuses on the areal extent of potential felsic material, identified based on a broad absorption feature centered at ~1.25-1.3 μm, a unique feature of feldspars attributed to minor Fe2+ substitution. These mapping efforts are put in geologic context using images from the High Resolution Imaging Science Experiment (HiRISE) instrument on MRO and existing mapping efforts in the area, as well as spectral context using laboratory generated spectra of feldspar and mafic mixtures. While further work understanding this potential felsic unit is warranted, if it is truly felsic it implies a more complicated Martian magmatic history than previously thought. As the diversity of known geologic materials on Mars grows, it is necessary that we understand how to recognize and characterize those materials using the instruments available on current and upcoming missions, such as MRO or the Mars 2020 Rover. Through modeling and data analysis, our ongoing work seeks to understand the geophysical and petrologic context in which the potential felsic materials were generated, and thus to infer their implications for Martian

  8. The Crustal Dichotomy Boundary West of Tempe Terra: Speculation on Where it Lies Beneath Alba Patera Based on Mola Topography

    NASA Technical Reports Server (NTRS)

    Frey, H.; Roark, J.; Sakimoto, S.; McGovern, P.

    1999-01-01

    MOLA gridded data based on profiles collected during the Aerobraking Hiatus and Science Phasing Operations suggest the crustal dichotomy boundary west of Tempe continues beneath Alba volcanics, at least to 105 W at about 50 N. A broad shelf-like region in the Alba units is continuous with a similar region of Tempe in which Hesperian volcanics overlie Noachian cratered terrain. Perspective views show significant changes in the sloping character of the flanks of Alba east and west of 105W, with much more continuous steep topography to the west. We suggest that Alba sits astride the ancient crustal dichotomy boundary, not adjacent to it, and that its eastern half lies on old cratered terrain. If true, this would significantly affect the estimate of Alba volcanics volumes, and might also explain some of the observed asymmetries in the structure and the distribution of faults associated with this immense feature.

  9. Scalloped terrains in the Peneus and Amphitrites Paterae region of Mars as observed by HiRISE

    NASA Astrophysics Data System (ADS)

    Lefort, A.; Russell, P. S.; Thomas, N.

    2010-01-01

    The Peneus and Amphitrites Paterae region of Mars displays large areas of smooth, geologically young terrains overlying a rougher and older topography. These terrains may be remnants of the mid-latitude mantle deposit, which is thought to be composed of ice-rich material originating from airfall deposition during a high-obliquity period less than 5 Ma ago. Within these terrains, there are several types of potentially periglacial features. In particular, there are networks of polygonal cracks and scalloped-shaped depressions, which are similar to features found in Utopia Planitia in the northern hemisphere. This area also displays knobby terrain similar to the so-called "basketball terrains" of the mid and high martian latitudes. We use recent high resolution images from the High Resolution Imaging Science Experiment (HiRISE) along with data from previous Mars missions to study the small-scale morphology of the scalloped terrains, and associated polygon network and knobby terrains. We compare these with the features observed in Utopia Planitia and attempt to determine their formation process. While the two sites share many general features, scallops in Peneus/Amphitrites Paterae lack the diverse polygon network (i.e. there is little variation in the polygon sizes and shapes) and large curvilinear ridges observed in Utopia Planitia. This points to a more homogeneous ice content within the substrate in the Peneus/Amphitrites Paterae region and implies that scallop formation is independent of polygon formation. This work shows that, as in Utopia Planitia, sublimation of interstitial ice is a likely process explaining the formation of the scalloped depressions in the region of Peneus/Amphitrites Paterae. Therefore, we provide a simplified scallop formation model based on sublimation of interstitial ice as proposed for Utopia Planitia. We also show that the differences in scallop morphologies between the two regions may be explained by differences in near-surface ice

  10. Hadriaca Patera

    NASA Technical Reports Server (NTRS)

    2002-01-01

    (Released 17 May 2002) The Science Although the largest volcanoes on Mars (and the solar system) are located in the geologically young Tharsis region, there are many other martian volcanoes that display equally interesting features, such as Hadriaca Patera, shown in this image. Hadriaca Patera is located to the northeast of the Hellas Planitia impact basin in the southern hemisphere. Unlike the Tharsis volcanoes, Hadriaca Patera has very low relief, standing only about 1-2 km above the surrounding plains. Many scientists believe that Hadriaca Patera and other patera volcanoes (e.g., Tyrrhena) had significant interaction with subsurface water that produced mostly explosive ash deposits (pyroclastic flows), rather than just lava flows. Nearby sources of water might have included Dao Vallis on the southern flank of the volcano. The upper portion of this image shows relatively smooth terrain located in the central caldera, which has been nearly filled in with late-stage lava flows. The lower half of the image shows lobate flows as well as furrows in the ash deposits that make up the volcano's southern flank; these erosional furrows may have formed by surface runoff or sapping by groundwater. Just below the center of the image, a few small sinuous troughs are visible, and may be collapsed lava tubes or collapse features related to subsurface water. The number of impact craters on a planetary surface is commonly used as a proxy for the age of the surface -- an old surface has had time to accumulate more craters than a young surface. The relatively small number of large craters in the image indicates that the surface in this area is younger than the nearby heavily cratered ancient terrains outside the Hellas basin, but there are more craters on this surface than would be found on the average volcanic surface in Tharsis (there are some very large old craters on the volcano's flank to the southeast of this image). Paterae in general are older than the Tharsis volcanoes. At

  11. Apollinaris Patera Erosion

    NASA Technical Reports Server (NTRS)

    2004-01-01

    18 September 2004 Apollinaris Patera is an ancient volcano located northwest of Gusev Crater, the landing site of the Mars Exploration Rover, Spirit. Apollinaris Patera, being rather old, is covered with craters, mantles of dust, and a wind-scoured covering of indurated, fine material. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a small portion of the Apollinaris Patera volcano, revealing the exhumation of older surfaces from beneath a relatively thin, wind-scoured material. This view is located on the upper south slope of the volcano, near 9.5oS, 186.4oW. The image covers an area approximately 3 km (1.9 mi) across and is illuminated by sunlight from the upper left.

  12. Deep Basalt Aquifers in Orcus Patera, Elysium Basin Mars: Perspectives for Exobiology Exploration

    NASA Technical Reports Server (NTRS)

    Grin, E. A.; Cabrol, N. A.

    1998-01-01

    Direct indicators of shorelines, spillways, and terraces allowed to determine the extent of the Elysium Paleolake between the contour-lines 1000 and 500 m below the Martian datum. The Elysium Paleolake is bordered north by Orcus Patera (14N/181W), which lies west of the Tartarus Montes and Tartarus Colles. The Orcus Patera displays an ellipse-shaped collapsed caldera of 360-km long and 100-km wide. Viking topographic data show that the bottom of the caldera is located at 2500 below the Martian datum, and surrounded by a steep-walled ram art which crest is located at about 0 m elevation. Considering the localization of Orcus Patera in the Elysium paleolake, its altimetry, and the magmatic origin of this caldera, we propose the existence of a paleolake in Orcus Patera generated (a) by juvenile water from magma during the Noachian period, and (b) by intermittent influx of the Elysium Basin from Hesperian to Amazonian. Results are encouraging to consider this site as a potential high-energy source environment for microbial communities. are circumscribed by a 50-km wide lava field mapped as Noachian material. The structure of Orcus Patera represents the record of material erupted from a magmatic reservoir. The caldera is enclosed by steep inner walls (25% measured from topographic data), values which could be in agreement with the presence of a deep magmatic reservoir, as suggested by the typology of Crumpler et.al. The depth of the caldera might be due to the collapse of the magma reservoir, and the release of gases accompanying the magma thermal evolution. Origins of water for the paleolake(s): The water that generated a paleolake in Orcus Patera may have come from two origins: (1) Juvenile water: Plescia and Crips estimated a magma H20 content by weight between 0.5% and 1.5% using for the first value a comparison with terrestrial basalt, and for the second values from a Martian meteorite. The amount of H20 can be estimated by the volume of erupted lava, and the lava

  13. Nili Patera

    NASA Technical Reports Server (NTRS)

    2003-01-01

    [figure removed for brevity, see original site]

    Released 14 May 2003

    At the summit of the low-relief shield volcano Syrtis Major, the caldera known as Nili Patera hosts a remarkable field of barchan-like dunes. The rugged knob to the north of the dunes is probably a breached volcanic cone representing one of the last eruptive events from this caldera.

    Image information: VIS instrument. Latitude 9, Longitude 67.4East (292.6). 19 meter/pixel resolution.

    Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.

    NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

  14. Meroe Patera

    NASA Technical Reports Server (NTRS)

    2002-01-01

    [figure removed for brevity, see original site]

    This image is located in Meroe Patera (longitude: 292W/68E, latitude: 7.01), which is a small region within Syrtis Major Planitia. Syrtis Major is a low-relief shield volcano whose lava flows make up a plateau more than 1000 km across. These flows are of Hesperian age (Martian activity of intermediate age) and are believed to have originated from a series of volcanic depressions, called calderas. The caldera complex lies on extensions of the ring faults associated with the Isidis impact basin toward the northeast - thus Syrtis Major volcanism may be associated with post-impact adjustments of the Martian crust.

    The most striking feature in this image is the light streaks across the image that lead to dunes in the lower left region. Wind streaks are albedo markings interpreted to be formed by aeolian action on surface materials. Most are elongate and allow an interpretation of effective wind directions. Many streaks are time variable and thus provide information on seasonal or long-term changes in surface wind directions and strengths. The wind streaks in this image are lighter than their surroundings and are the most common type of wind streak found on Mars. These streaks are formed downwind from crater rims (as in this example), mesas, knobs, and other positive topographic features.

    The dune field in this image is a mixture of barchan dunes and transverse dunes. Dunes are among the most distinctive aeolian feature on Mars, and are similar in form to barchan and transverse dunes on Earth. This similarity is the best evidence to indicate that martian dunes are composed of sand-sized material, although the source and composition of the sand remain controversial. Both the observations of dunes and wind streaks indicate that this location has a windy environment - and these winds are persistent enough to product dunes, as sand-sized material accumulates in this region. These features also indicate that the

  15. Loki Patera

    NASA Technical Reports Server (NTRS)

    1983-01-01

    A huge area of Io's volcanic plains is shown in this Voyager 1 image mosaic. Numerous volcanic calderas and lava flows are visible here. Loki Patera, an active lava lake, is the large shield-shaped black feature. Heat emitted from Loki can be seen through telescopes all the way from Earth. These telescopic observations tell us that Loki has been active continuously (or at least every time astronomers have looked) since the Voyager 1 flyby in March 1979. The composition of Io's volcanic plains and lava flows has not been determined, but they could consist dominantly of sulfur with surface frosts of sulfur dioxide or of silicates (such as basalts) encrusted with sulfur and sulfur dioxide condensates. The bright whitish patches probably consist of freshly deposited SO2 frost. The black spots, including Loki, are probably hot sulfur lava, which may remain molten by intrusions of molten silicate magma, coming up from deeper within Io. The ultimate source of heat that keeps Io active is tidal frictional heating due to the continual flexure of Io by the gravity of Jupiter and Europa, another of Jupiter's satellites.

  16. Ulysses Patera

    NASA Technical Reports Server (NTRS)

    2002-01-01

    [figure removed for brevity, see original site] (Released 18 July 2002) It is helpful to look at the context for this THEMIS image, which covers a large area over the summit of Ulysses Patera. Ulysses Patera is one of the many volcanoes that make up the giant Tharsis volcanic province, although Ulysses itself is fairly small in comparison to the other volcanoes in this area. In the context image, there are 3 circular features near the top of the volcano. The large, central feature is called a 'caldera', and is the result of volcanic activity at Ulysses. The other two circular features are impact craters. The THEMIS image primarily spans across the central caldera, but also covers a portion of the northernmost impact crater. We know that the large central caldera must have formed earlier than the two craters, because its circular form has been cut by the smaller crater rims. In the THEMIS image, there are stair-stepping plateaus in the northern portion of the image. These are part of the rim of the northern crater, and are caused by collapse or subsidence after the impact event. Just to the south of this crater, 'rayed' patterns can be seen on part of the caldera floor. The rayed pattern is most likely due to a landslide of material down the crater rim slope. Another possibility is that the impact that formed the northern crater caused material to be ejected radially, and then parts of the ejecta have either been buried or eroded away. Other signs of mass movement events in this image are dark streaks, caused by dust avalanches, visible in the caldera's northern wall. In the central portion of the image, there are two lobe-shaped features-one overlaps the other-that appear to have flowed westward. It is likely that these features are ejecta lobes, because they are located adjacent to the southeastern crater (see context image). The fluidized appearance of these ejecta lobes is probably due to a significant amount of ice or water being present in the soil at the time

  17. The Keck "Mars 2000" Project: Using Mars Orbiter Laser Altimeter Data to Assess Geological Processes and Regional Stratigraphy Near Orcus Patera and Marte Vallis on Mars

    NASA Technical Reports Server (NTRS)

    Grosfils, E. B.; Sakimoto, S. E. H.; Mendelson, C. V.; Bleacher, J. E.

    2001-01-01

    During the Keck 'Mars 2000' summer project 10 undergraduates (rising juniors) used Mars Orbiter Laser Altimeter (MOLA) data to study a 19x14 degree region they identified as a potential Mars 2003 landing site. Here we introduce the project science and organization. Additional information is contained in the original extended abstract.

  18. Inversion of Gravity and Magnetic Field Data for Tyrrhena Patera

    NASA Technical Reports Server (NTRS)

    Milbury, C.; Schubert, G.; Raymond, C. A.; Smrekar, S. E.

    2011-01-01

    Tyrrhena Patera is located to the southeast/northeast of the Isidis/Hellas impact basin. It was geologically active into the Late Amazonian, although the main edifice was formed in the Noachian(approximately 3.7-4.0 Ga). Tyrrhena Patera and the surrounding area contain gravity and magnetic anomalies that appear to be correlated. The results presented here are for the anomalies 1a and 1b (closest to Tyrrhena Patera), however other anomalies in this region have been modeled and will be presented at the conference.The Mars Global Surveyor (MGS) free-air gravity signature of Tyrrhena Patera has been studied by Kiefer, who inferred the existence of an extinct magma chamber below it. The magnetic signature has been mapped by Lillis R. J. et al., who compared electron reflectometer data, analogous to the total magnetic field, for Syrtis Major and Tyrrhena Patera and argued for demagnetization of both volcanoes.

  19. Nili Patera Dune Field

    NASA Technical Reports Server (NTRS)

    2005-01-01

    [figure removed for brevity, see original site]

    Our topic for the weeks of April 4 and April 11 is dunes on Mars. We will look at the north polar sand sea and at isolated dune fields at lower latitudes. Sand seas on Earth are often called 'ergs,' an Arabic name for dune field. A sand sea differs from a dune field in two ways: 1) a sand sea has a large regional extent, and 2) the individual dunes are large in size and complex in form.

    This VIS image shows a dune field within Nili Patera, the northern caldera of a large volcanic complex in Syrtis Major.

    Image information: VIS instrument. Latitude 9, Longitude 67 East (293 West). 19 meter/pixel resolution.

    Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.

    NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

  20. Quantitative studies of volcanic processes on Mars using data from the Mars Global Surveyor

    NASA Astrophysics Data System (ADS)

    Bishop, Louise Jane

    Volcanic processes on Mars were investigated using topographic profiles derived with the help of IDL software from data collected by the Mars Orbiter Laser Altimeter (MOLA) on the Mars Global Surveyor Mission (MGS) in 1997-2001 and images obtained by the MGS Mars Orbiter Camera (MOC) and by the earlier Viking mission. Thickness and slope values for lava flows at both Elysium Mons and Alba Patera made it possible to compute flow emplacement times and effusion rates using the flow growth model proposed by C. R. J. Kilburn and R. M. C Lopes in 1990. Geological mapping of the Elysium volcanic region showed that Elysium Mons was emplaced as a result of a single shift in vent position on top of an older volcanic edifice, here termed the Ancient Volcanic Edifice (AVE). This implies that there have been substantial variations in both position and time for the magma supply. Calculations suggest that the flows at Alba Patera were emplaced more quickly than those at Elysium Mons, possibly owing to differences in fissure width and lava composition. There is evidence for both aa and pahoehoe on the summit areas of Elysium Mons and Alba Patera. The presence of aa is consistent with the view that long lava flows on Mars are emplaced quickly. Pahoehoe flows imply slow emplacement, and their inferred presence on Mars provides support for the theory that long terrestrial lavas are often emplaced as sheets of inflated pahoehoe. MOC image analysis indicated that late-stage explosive activity has occurred at several Martian volcanoes where it was previously undetected, contrary to the prevalent view that Martian volcanism evolves from explosive to effusive activity. To resolve the many ambiguities inherent in morphological data and imagery the need remains for ground truthing by experienced observers and detailed geochemical analyses in situ or by means of a sample return mission

  1. The gravity field of Mars: results from Mars Global Surveyor.

    PubMed

    Smith, D E; Sjogren, W L; Tyler, G L; Balmino, G; Lemoine, F G; Konopliv, A S

    1999-10-01

    Observations of the gravity field of Mars reveal a planet that has responded differently in its northern and southern hemispheres to major impacts and volcanic processes. The rough, elevated southern hemisphere has a relatively featureless gravitational signature indicating a state of near-isostatic compensation, whereas the smooth, low northern plains display a wider range of gravitational anomalies that indicates a thinner but stronger surface layer than in the south. The northern hemisphere shows evidence for buried impact basins, although none large enough to explain the hemispheric elevation difference. The gravitational potential signature of Tharsis is approximately axisymmetric and contains the Tharsis Montes but not the Olympus Mons or Alba Patera volcanoes. The gravity signature of Valles Marineris extends into Chryse and provides an estimate of material removed by early fluvial activity.

  2. Io: Heat flow from dark paterae

    NASA Astrophysics Data System (ADS)

    Veeder, Glenn J.; Davies, Ashley Gerard; Williams, David A.; Matson, Dennis L.; Johnson, Torrence V.; Radebaugh, Jani

    2011-03-01

    Dark paterae on the jovian satellite Io are evidence of recent volcanic activity. Some paterae appear to be entirely filled with dark volcanic material, while others have only partially darkened floors. Dark paterae have area and heat flow longitudinal distributions that are bimodal as well as anti-correlated with the longitudinal distribution of mountains on Io at a global scale. As part of our study of Io’s total heat flow, we have examined the darkest paterae and quantified their thermal emission in order to assess their contribution. This is the first time that the areas of the dark material in these paterae have been measured with such precision and correlated with their thermal emission. Dark paterae yield a significantly larger contribution to Io’s heat flow than dark volcanic fields. Dark paterae (including Loki Patera) yield at least ∼4 × 1013 W or ∼40% of Io’s total heat flow. In comparison, dark flow fields yield ∼1013 W or ∼10% of Io’s total heat flow. Of the total heat loss from dark paterae, Loki Patera alone yields ∼1013 W or ∼10% of Io’s total thermal emission.

  3. Apollinaris Patera: An Early Martian Mantle Plume?

    NASA Astrophysics Data System (ADS)

    Kiefer, W. S.

    2015-12-01

    Apollinaris Patera is one of the largest volcanos on Mars outside of the Tharsis volcanic province (summit relief 5.4 km, volume 7.3x1013 m3). The mapped crater densities on Apollinaris indicate that volcanic activity ended 3.5 to 3.8 billion years ago. Apollinaris is located on the northern (lowland) side of the martian hemispheric dichotomy. Because it is an isolated, relatively point-like source of volcanism, it is plausibly interpreted as an early example of a martian mantle plume. Plume structure and conditions in the mantle can be constrained using finite element mantle convection simulations combined with a variety of petrological, geophysical, and geologic observations. (1) Basalts studied by the MER Spirit rover in nearby Gusev crater are similar in age and possibly physically connected to Apollinaris Patera. Petrologic modeling of the Gusev crater basalt compositions indicates that the thermal lithosphere was about 100 km thick with a mantle potential temperature of 1480-1530 °C. This requires a mantle thermal Rayleigh number of about 2x108 at the time of volcanism, based on the volume-averaged mantle viscosity. (2) Pyroclastic deposits at Apollinaris indicate that at least a portion of the volcanism occurred in the presence of a high concentration of water or other volatiles. This lowers the solidus temperature and increases the magma production rate but has only a limited effect on the minimum depth of melting. (3) There is a localized magnetic anomaly beneath Apollinaris that indicates that the martian core dynamo persisted until at least the earliest stage of Apollinaris volcanism, which in turn sets a lower bound on the core heat flux of 5-10 mW m-2. Preservation of the magnetic field may be the result of formation of magnetic minerals such as magnetite due to volcanically-driven hydrothermal alteration of crustal rocks beneath Apollinaris.

  4. Assessment of antipodal-impact terrains on Mars

    NASA Technical Reports Server (NTRS)

    Williams, David A.; Greeley, Ronald

    1994-01-01

    The regions anitpodal to Mars' three largest impact basins, Hellas, Isidis, and Argyre, were assessed for evidence of impact-induced disrupted terrains. Photogeology and computer modeling using the Simplified Arbitrary Lagrangian Eulerian (SALE) finite element code suggest that such terrains could have been found by the Hellas impact. Maximum antipodal pressures are 1100 MPa for Hellas, 520 MPa for Isidis, and 150 MPa for Argyre. The results suggest that if antipodal fracturing were associated with later volcanism, then Alba Patera may be related to the Hellas event, as proposed by Peterson (1978). Alba Patera is a unique volcano in the solar system, being a shield volcano which emitted large volume lava flows. This volcanism could be the result of the focusing of seismic energy which created a fractured region that served as a volcanic conduit for the future release of large volumes of magma. No disrupted terrain features are observed antipodal to the Isidis or Argyre basins, although some of the old fractures in Noctis Labyrinthus could have originated in response to the Isidis impact, and later have been reactivated by the Tharsis tectonics assumed to have produced Noctis. If the lower calculated antipodal pressures for Argyre were capable of producing disrupted terrains, then the terrains have been covered subsequently by volcanic or aeolian material, or modified beyond recognition.

  5. Rheological analyses of lava flows on Mars

    NASA Technical Reports Server (NTRS)

    Moore, H. J.; Davis, P. A.

    1991-01-01

    Researchers obtained 183 profiles of lava flows on Mars using photoclinometry. These photoclinometric profiles were leveled by adjusting them until the levee crests or bases had the same elevations (depending on the situation). Here, researchers report some of the results of their analysis of 27 flows on the flanks of Alba Patera (3 flows), near the summit of Ascraeus Mons (6 flows), the flanks of Arsia Mons (3 flows), and the flanks of Olympus Mons (15 flows). Results suggest that the flows examined to date are not felsic or ultramafic; rather, they probably range from basalts to basaltic andesites. Thus, the suggestion that flows on Olympus Mons and elsewhere may be more silicic than Hawaiian basalts is supported by the researchers' results. These suggestions are testable with suitable measurements of silica contents of the flows.

  6. Resurfacing History of Vastitas Borealis, Mars: Early Amazonian Climate Implications

    NASA Astrophysics Data System (ADS)

    Tanaka, K. L.

    2001-12-01

    Geologic mapping of the north polar plains of Mars (>60° N.), aka Vastitas Borealis, based on Mars Orbiter Laser Altimeter (MOLA) topography, reveals new insights into resurfacing events in the polar region during the Amazonian Period. Deposits making up the Vastitas Borealis Formation (VBF) were emplaced at the end of the Hesperian Period and covered this entire region except for lavas of northernmost Alba Patera. No evidence for a Hesperian polar plateau has been found, although Planum Boreum could bury such evidence. A plains deposit, the Scandia unit, ranges from 20 to 200 m thick and overlies the VBF between Alba Patera and Olympia Planitia. This unit is apparently friable, because it is preserved only as eroded remnants forming knobs and mesas, including those of Scandia Colles. The VBF and Scandia units both appear to be deformed by radial tilting and concentric folding of Alba Patera. Another deposit, the Boreum unit, forms the base of Planum Boreum and possibly high-standing knobs and mesas south of Chasma Boreale and underlies the evenly bedded polar layered deposits. MOC images and MOLA data reveal that this unit has irregular bedding, locally steep scarps, and a dark color and is interpreted by S. Byrne and B. Murray (personal commun.) as a frozen sand sea. The unit may be up to a kilometer thick along the margins of Chasma Boreale and thins out away from there, possibly underlying the northern, southward-sloping ejecta of a 24 km crater at 79° N., 299° W. Potentially, the Scandia and Boreum units could be remnants of a single deposit. Within Chasma Boreale, the chasma unit forms a tongue-shaped plateau as much as 350 m thick. This unit could be a lower section of the Boreum unit, but a lack of relict knobs or mesas on its surface suggests that the unit embays the Boreum unit instead. South of Olympia Planitia, the Scandia unit becomes difficult to trace, and volcanic-like forms possibly related to eruption of material and subsequent collapse and

  7. Pityriasis Alba

    MedlinePlus

    ... Annual Meeting 2013 OMED Schedule Needs Assessments Speaker Bios Meeting Feedback 2014 Midyear Meeting Attestation 2014 Midyear ... to go away by adulthood. The loss of pigment associated with pityriasis alba is not permanent. Diagnosis ...

  8. Colors and Volatile Deposition Around Loki Patera

    NASA Astrophysics Data System (ADS)

    Morgan, R. S.; Howell, R. R.

    2007-03-01

    To evaluate the role of volatiles at Loki Patera we are reprocessing Galileo images to obtain the highest spatial resolution color information available, and comparing the resulting spectra to candidate materials and other regions on Io.

  9. Temperature and variability of Pillan, Wayland Patera, and Loki Patera on Io from Cassini ISS data

    NASA Astrophysics Data System (ADS)

    Allen, Daniel R.; Radebaugh, Jani; Stephens, Denise C.

    2013-09-01

    Cassini spacecraft images of Io obtained during its flyby of Jupiter in late 2000 and early 2001 were used to determine the lava composition and eruption style of three faint hot spots, Pillan, Wayland Patera, and Loki Patera. We found a maximum color temperature of 1130 ± 289 K for Pillan and maximum color temperatures of 1297 ± 289 K and 1387 ± 287 K for Wayland Patera and Loki Patera, respectively. These temperatures are suggestive of basaltic lava but an ultramafic composition cannot be ruled out. The temperatures with the best signal-to-noise ratios also suggested basaltic lava and were found to be 780 ± 189 K, 1116 ± 250 K, and 1017 ± 177 K for Pillan, Wayland Patera, and Loki Patera, respectively. Pillan showed constant thermal output within error over three days of observations. The data also suggest Pillan may be surrounded by topography that blocked emission in the middle of the observation and caused a more dramatic decrease in emission. Wayland Patera’s intensity decreased over the three eclipse observations, consistent with a cooling lava flow or decreasing effusion rate. Intensities at Loki Patera over the course of the observations varied, consistent with previous determinations that Loki Patera is an often quiescent lava lake with periods of overturning, fountaining, and crustal foundering.

  10. Sand Dunes of Nili Patera in 3-D

    NASA Technical Reports Server (NTRS)

    2001-01-01

    The most exciting new aspect of the Mars Global Surveyor (MGS) Extended Mission is the opportunity to turn the spacecraft and point the Mars Orbiter Camera (MOC) at specific features of interest. Opportunities to point the spacecraft come about ten times a week. Throughout the Primary Mission (March 1999 - January 2001), nearly all MGS operations were conducted with the spacecraft pointing 'nadir'--that is, straight down. A search for the missing Mars Polar Lander in late 1999 and early 2000 demonstrated that pointing the spacecraft could allow opportunities for MOC to see things that simply had not entered its field of view during typical nadir-looking operations, and to target areas previously seen in a nadir view so that stereo ('3-D') pictures could be derived.

    One of the very first places photographed by the MOC at the start of the Mapping Mission in March 1999 was a field of dunes located in Nili Patera, a volcanic depression in central Syrtis Major. A portion of this dune field was shown in a media release on March 11, 1999, 'Sand Dunes of Nili Patera, Syrtis Major'. Subsequently, the image was archived with the NASA Planetary Data System, as shown in the Malin Space Science Systems MOC Gallery. On April 24, 2001, an opportunity arose in which the MGS could be pointed off-nadir to take a new picture of the same dune field. By combining the nadir view from March 1999 and the off-nadir view from April 2001, a stereoscopic image was created. The anaglyph shown here must be viewed with red (left-eye) and blue (right-eye) '3-D' glasses. The dunes and the local topography of the volcanic crater's floor stand out in sharp relief. The images, taken more than one Mars year apart, show no change in the shape or location of the dunes--that is, they do not seem to have moved at all since March 1999.

  11. Lunar and Planetary Science XXXV: Mars Volcanology and Tectonics

    NASA Technical Reports Server (NTRS)

    2004-01-01

    Reports from the session, "Mars Volcanology and Tectonics" include:Martian Shield Volcanoes; Estimating the Rheology of Basaltic Lava Flows; A Model for Variable Levee Formation Rates in an Active Lava Flow; Deflections in Lava Flow Directions Relative to Topography in the Tharsis Region: Indicators of Post-Flow Tectonic Motion; Fractal Variation with Changing Line Length: A Potential Problem for Planetary Lava Flow Identification; Burfellshraun:A Terrestrial Analogue to Recent Volcanism on Mars; Lava Domes of the Arcadia Region of Mars; Comparison of Plains Volcanism in the Tempe Terra Region of Mars to the Eastern Snake River Plains, Idaho with Implications for Geochemical Constraints; Vent Geology of Low-Shield Volcanoes from the Central Snake River Plain, Idaho: Lessons for Mars and the Moon; Field and Geochemical Study of Table Legs Butte and Quaking Aspen Butte, Eastern Snake River Plain, Idaho: An Analog to the Morphology of Small Shield Volcanoes on Mars; Variability in Morphology and Thermophysical Properties of Pitted Cones in Acidalia Planitia and Cydonia Mensae; A Volcano Composed of Light-colored Layered Deposits on the Floor of Valles Marineris; Analysis of Alba Patera Flows: A Comparison of Similarities and Differences Geomorphologic Studies of a Very Long Lava Flow in Tharsis, Mars; Radar Backscatter Characteristics of Basaltic Flow Fields: Results for Mauna Ulu, Kilauea Volcano, Hawaii;and Preliminary Lava Tube-fed Flow Abundance Mapping on Olympus Mons.

  12. Venus - Sag Caldera 'Sachs Patera

    NASA Technical Reports Server (NTRS)

    1991-01-01

    This image of Sachs Patera on Venus is centered at 49 degrees north, 334 degrees east. Defined as a sag-caldera, Sachs is an elliptical depression 130 meters (81 feet) in depth, spanning 40 kilometers (25 miles) in width along its longest axis. The morphology implies that a chamber of molten material drained and collapsed, forming a depression surrounded by concentric scarps spaced 2-to-5 kilometers (1.2- to-3 miles) apart. The arc-shaped set of scarps, extending out to the north from the prominent ellipse, is evidence for a separate episode of withdrawal; the small lobe-shaped extension to the southwest may represent an additional event. Solidified lava flows 10-to-25 kilometers (6-to-16 miles) long, give the caldera its flower-like appearance. The flows are a lighter tone of gray in the radar data because the lava is blockier in texture and consequently returns more radar waves. Much of the lava, which was evacuated from the chamber, probably traveled to other locations underground, while some of it may have surfaced further south. This is unlike calderas on Earth, where a rim of lava builds up in the immediate vicinity of the caldera.

  13. Topography of Apollinaris Patera and Ma'adim Vallis

    NASA Technical Reports Server (NTRS)

    Thornhill, G. D.; Rothery, D. A.; Murray, J. B.; Day, T.; Cook, A.; Muller, J.-P.; Iliffe, J. C.

    1992-01-01

    Digital elevation models of the northern part of Ma'adim Vallis (603a41 607m/pix, 639a91 721m/pix), and Apollinaris Patera (603a42 612m/pix, 639a92 717m/pix), covering the area between 180 degrees to 190 degrees long and -2 degrees to -20 degrees lat. were obtained using a method described here. The results for the Ma'adim Vallis area show broad agreement with the United States Geological Survey (USGS) topographic map of the area with a channel depth of 1 to 2 km. A detailed study of the variations in the channel depth along its course and calculations of its discharge rate from channel cross section and slope are currently being undertaken. Results for Apollinaris Patera have been obtained, although the absolute heights relative to the Mars datum are not well constrained. However, the relative heights are sufficient for some analysis. Again, the topographic map is in reasonable agreement with the USGS map of the area, although there are significant differences.

  14. The Seasonal Behavior of Water Ice Clouds in the Tharsis and Valles Marineris Regions of Mars: Mars Orbiter Camera Observations

    NASA Technical Reports Server (NTRS)

    Benson, J. L.; Bonev, B. P.; James, P. B.; Shan, K. J.; Cantor, B. A.; Caplinger, M. A.

    2003-01-01

    The Mars Orbiter Camera (MOC) was used to obtain global maps of the Martian surface. The maps used were acquired between March 15, 1999 (LS = 110 ) and July 31, 2001 (L(sub s) = 110), corresponding to approximately one and a quarter martian years. In this work we focused on water ice clouds associated with the surface features of Olympus Mons, Ascraeus Mons, Pavonis Mons, Arsia Mons, Alba Patera, and the Valles Marineris canyon system. Using these data, we have made three types of quantitative measurements to characterize the cloud activity: 1) cloud area and location, 2) cloud height, and 3) cloud optical depth. We have also searched for short period variations in the cloud areas.

  15. The formation of antipodal-impact terrains on Mars

    NASA Technical Reports Server (NTRS)

    Williams, D. A.; Greeley, Ronald

    1991-01-01

    The regions antipodal to Mars' three largest impact basins, Hellas, Isidis, and Argyre, were assessed for evidence of impact induced seismically disrupted terrains. Photogeology and preliminary computer modeling using the Simplified Arbitrary Lagrangian-Eulerian computer program suggest such terrain could have been formed by the Hellas and Isidis impacts. Previously, the only assessment of potential surface disruptions on Mars antipodal to large impacts was by Peterson (1978). Herein, the results give credence to Peterson's assertions. For Hellas, the computer model clearly suggests that antipodal pressures were probably strong enough to have fractured the crust and disrupted the surface, and may account for aspects of volcanism at Alba Patera. It is suggested that the Hellas impact produced sufficient focused energy at its antipode to produce deep fracture in the Martian crust centered below the current caldera for Alba Petera. With the generation and evolution of magma in the Tharsis area, the fracture system provided a ready conduit for early stage eruptions of Martians lavas derived from deep in the crust and/or upper mantle, perhaps of komatiitic composition.

  16. Venus - A Large Elongated Caldera 'Sacajawea Patera

    NASA Technical Reports Server (NTRS)

    1991-01-01

    This Magellan image reveals Sacajawea Patera, a large, elongate caldera located in Western Ishtar Terra on the smooth plateau of Lakshmi Planum. The image is centered at 64.5 degrees North latitude and 337 degrees East longitude. It is approximately 420 kilometers (252 miles) wide at the base. Sacajawea is a depression approximately 1-2 kilometers (0.6-1.2 miles) deep and 120 x 215 kilometers (74 x 133 miles) in diameter; it is elongate in a southwest-northeast direction. The depression is bounded by a zone of circumferential curvilinear structures interpreted to be graben and fault scarps. These structures are spaced 0.5-4 kilometers (0.3-2.5 miles) apart, are 0.6-4.0 kilometers (0.4-2.5 miles) in width and up to 100 kilometers (62 miles) in length. Extending up to approximately 140 kilometers (87 miles) in length from the southeast of the patera is a system of linear structures thought to represent a flanking rift zone along which the lateral injection and eruption of magma may have occurred. A shield edifice 12 kilometers (7 miles) in diameter with a prominent central pit lies along the trend of one of these features. The impact crater Zlata, approximately 6 kilometers (4 miles) in diameter is located within the zone of graben to the northwest of the patera. Few flow features are observed in association with Sacajawea, possibly due to age and state of degradation of the flows. Mottled bright deposits 4-20 kilometers (2.5-12 miles) in width are located near the periphery and in the center of the patera floor within local topographic lows. Diffuse patches of dark material approximately 40 kilometers (25 miles) in width are observed southwest of the patera, superposed on portions of the surrounding graben. The formation of Sacajawea is thought to be related to the drainage and collapse of a large magma chamber. Gravitational relaxation may have caused the resultant caldera to sag, producing the numerous faults and graben that circumscribe the patera. Regions of

  17. Io: Loki Patera as a Magma Sea

    NASA Technical Reports Server (NTRS)

    Matson, Dennis L.; Davies, Ashley Gerard; Veeder, Glenn J.; Rathbun, Julie A.; Johnson, Torrence V.; Castillo, Julie C.

    2006-01-01

    We develop a physical model for Loki Patera as a magma sea. We calculate the total volume of magma moving through the Loki Patera volcanic system every resurfacing cycle (approx.540 days) and the resulting variation in thermal emission. The rate of magma solidification at times reaches 3 x 10(exp 6) kg per second, with a total solidified volume averaging 100 cu km per year. A simulation of gas physical chemistry evolution yields the crust porosity profile and the timescale when it will become dense enough to founder in a manner consistent with observations. The Loki Patera surface temperature distribution shows that different areas are at different life cycle stages. On a regional scale, however, there can be coordinated activity, indicated by the wave of thermal change which progresses from Loki Patera's SW quadrant toward the NE at a rate of approx.1 km per day. Using the observed surface temperature distribution, we test several mechanisms for resurfacing Loki Patera, finding that resurfacing with lava flows is not realistic. Only the crustal foundering process is consistent with observations. These tests also discovered that sinking crust has a 'heat deficit' which promotes the solidification of additional magma onto the sinking plate ("bulking up"). In the limiting case, the mass of sinking material can increase to a mass of approx.3 times that of the foundering plate. With all this solid matter sinking, there is a compensating upward motion in the liquid magma. This can be in excess of 2 m per year. In this manner, solid-liquid convection is occurring in the sea.

  18. Mars - Thickness of the lithosphere from the tectonic response to volcanic loads

    NASA Technical Reports Server (NTRS)

    Comer, R. P.; Solomon, S. C.; Head, J. W.

    1985-01-01

    The response to loading of the elastic lithosphere of Mars by seven large volcanic features is estimated based on the hypothesis of a flexural origin for a definable set of load-concentric graben. From the locations of such graben, or from their absence, the lithospheric thickness and flexural rigidity are inferred. For the Tharsis montes, Alba Patera, and Elysium Mons, elastic lithospheric thicknesses at the time of loading range from 20 to 50 km, assuming a Young's modulus of a trillion dyn/sq cm. The thickness exceeded 120 km beneath Olympus Mons and Isidis Planitia. The corresponding ranges in flexural rigidity are approximately 10 to the 30th to 31st dyn cm and greater than 10 to the 32nd dyn cm, respectively. These results indicate a local thinning of the lithosphere beneath portions of the central regions of the Tharsis and Elysium volcanic provinces at the time of loading-induced fracturing.

  19. Maps of Mars Global Topography

    NASA Technical Reports Server (NTRS)

    1999-01-01

    Maps of Mars' global topography. The projections are Mercator to 70o latitude and stereographic at the poles with the south pole at left and north pole at right. Note the elevation difference between the northern and southern hemispheres. The Tharsis volcano-tectonic province is centered near the equator in the longitude range 220o E to 300o E and contains the vast east-west trending Valles Marineris canyon system and several major volcanic shields including Olympus Mons (18o N, 225o E), Alba Patera (42o N, 252o E), Ascraeus Mons (12o N, 248o E), Pavonis Mons (0o, 247o E), and Arsia Mons (9o S, 239o E). Regions and structures discussed in the text include Solis Planum (25o S, 270o E), Lunae Planum (10o N, 290o E), and Claritas Fossae (30o S, 255o E). Major impact basins include Hellas (45o S, 70o E), Argyre (50o S, 320o E), Isidis (12o N, 88o E), and Utopia (45o N, 110o E). This analysis uses an areocentric coordinate convention with east longitude positive.

  20. Loki Patera: A Magma Sea Story

    NASA Technical Reports Server (NTRS)

    Veeder, G. J.; Matson, D. L.; Rathbun, A. G.

    2005-01-01

    We consider Loki Patera on Io as the surface expression of a large uniform body of magma. Our model of the Loki magma sea is some 200 km across; larger than a lake but smaller than an ocean. The depth of the magma sea is unknown, but assumed to be deep enough that bottom effects can be ignored. Edge effects at the shore line can be ignored to first order for most of the interior area. In particular, we take the dark material within Loki Patera as a thin solidified lava crust whose hydrostatic shape follows Io's isostatic surface (approx. 1815 km radius of curvature). The dark surface of Loki appears to be very smooth on both regional and local (subresolution) scales. The thermal contrast between the low and high albedo areas within Loki is consistent with the observed global correlation. The composition of the model magma sea is basaltic and saturated with dissolved SO2 at depth. Its average, almost isothermal, temperature is at the liquidus for basalt. Additional information is included in the original extended abstract.

  1. Primary centers and secondary concentrations of tectonic activity through time in the western hemisphere of Mars

    USGS Publications Warehouse

    Anderson, R.C.; Dohm, J.M.; Golombek, M.P.; Haldemann, A.F.C.; Franklin, B.J.; Tanaka, K.L.; Lias, J.; Peer, B.

    2001-01-01

    Five main stages of radial and concentric structures formed around Tharsis from the Noachian through the Amazonian as determined by geologic mapping of 24,452 structures within the stratigraphic framework of Mars and by testing their radial and concentric orientations. Tectonic activity peaked in the Noachian (stage 1) around the largest center, Claritas, an elongate center extending more than 20?? in latitude and defined by about half of the total grabens which are concentrated in the Syria Planum, Thaumasia, and Tempe Terra regions. During the Late Noachian and Early Hesperian (stage 2), extensional structures formed along the length of present-day Valles Marineris and in Thaumasia (with a secondary concentration near Warrego Vallis) radial to a region just to the south of the central margin of Valles Marineris. Early Hesperian (stage 3) radial grabens in Pavonis, Syria, Ulysses, and Tempe Terra and somewhat concentric wrinkle ridges in Lunae and Solis Plana and in Thaumasia, Sirenum, Memnonia, and Amazonis are centered northwest of Syria with secondary centers at Thaumasia, Tempe Terra, Ulysses Fossae, and western Valles Marineris. Late Hesperian/Early Amazonian (stage 4) structures around Alba Patera, the northeast trending alignment of Tharsis Montes, and Olympus Mons appears centered on Alba Patera. Stage 5 structures (Middle-Late Amazonian) represent the last pulse of Tharsis-related activity and are found around the large shield volcanoes and are centered near Pavonis Mons. Tectonic activity around Tharsis began in the Noachian and generally decreased through geologic time to the Amazonian. Statistically significant radial distributions of structures formed during each stage, centered at different locations within the higher elevations of Tharsis. Secondary centers of radial structures during many of the stages appear related to previously identified local magmatic centers that formed at different times and locations throughout Tharsis. Copyright 2001 by

  2. Tidally-controlled volcanism at Loki Patera, Io?

    NASA Astrophysics Data System (ADS)

    Rhoden, A. R.; Kite, E. S.

    2011-10-01

    We compare the time-varying thermal emission from Io's Loki Patera to calculations of tidal stress caused by Io's orbital eccentricity. Our preliminary analysis supports the hypothesis that tidal stresses influence the timing of Loki emission.

  3. Two New Brightening Events at Io's Loki Patera

    NASA Astrophysics Data System (ADS)

    de Kleer, K.; De Pater, I.

    2015-12-01

    Loki Patera is one of the most dramatically time-variable volcanic features on Io, exhibiting periodic brightening events every 1-2 years that constitute over 15% of Io's global heat flow when active. We obtained new near-infrared (2-5 μm) observations of Loki Patera on 37 nights during and after two such brightening events using adaptive optics at the Keck and Gemini North telescopes in 2013-2015. We modify the Matson et al. (2006) model for Loki Patera as an overturning basaltic magma sea to model our observations, and find an overturn front propagation velocity of 0.85-0.95 km/day. The 445±45 day interval between the two events is 100 days shorter than the 540-day period calculated by Rathbun et al. (2002) for events prior to 2001. The overturn front appears to propagate around the patera in the clockwise direction, opposite to what has been inferred for these past brightening events, and may include irregular propagation patterns and multiple simultaneous fronts. Based on the anomalously-low intensities when Loki Patera is viewed at high emission angle, we find evidence for a topographic barrier to the west of the patera, which may be a raised region or the edge of a depression in which the magma sea resides.

  4. Dielectric properties of lava flows west of Ascraeus Mons, Mars

    USGS Publications Warehouse

    Carter, L.M.; Campbell, B.A.; Holt, J.W.; Phillips, R.J.; Putzig, N.E.; Mattei, S.; Seu, R.; Okubo, C.H.; Egan, A.F.

    2009-01-01

    The SHARAD instrument on the Mars Reconnaissance Orbiter detects subsurface interfaces beneath lava flow fields northwest of Ascraeus Mons. The interfaces occur in two locations; a northern flow that originates south of Alba Patera, and a southern flow that originates at the rift zone between Ascraeus and Pavonis Montes. The northern flow has permittivity values, estimated from the time delay of echoes from the basal interface, between 6.2 and 17.3, with an average of 12.2. The southern flow has permittivity values of 7.0 to 14.0, with an average of 9.8. The average permittivity values for the northern and southern flows imply densities of 3.7 and 3.4 g cm-3, respectively. Loss tangent values for both flows range from 0.01 to 0.03. The measured bulk permittivity and loss tangent values are consistent with those of terrestrial and lunar basalts, and represent the first measurement of these properties for dense rock on Mars. Copyright 2009 by the American Geophysical Union.

  5. Mars Crustal Magnetism: Plate Tectonics and Flood Basalts

    NASA Astrophysics Data System (ADS)

    Connerney, J.; Acuna, M.; Ness, N.

    2006-12-01

    The crustal magnetic field of Mars, mapped in unprecedented detail by the Mars Global Surveyor spacecraft, bears a record of crustal formation and subsequent evolution. The magnetic field in Meridiani has characteristics (transform faulting, symmetry) associated with crustal spreading in the presence of a reversing dynamo. The detailed erasure of crustal fields in and around filled basins (Utopia, Isidis) and massive volcanic constructs (Tharsis Montes, Oylmpus Mons, Alba Patera, Elysium Mons) suggests that the northern plains were largely demagnetized by emplacement of ~km thick flood basalts in single cooling events. Thermal demagnetization under a few km of flood basalts would require that the pre-existing magnetic imprint be borne in a layer only a few km thick. This in turn implies very intense magnetization (order 100 A/m) if the same layer thickness is applied to the intensely magnetized southern highlands. Icelandic basalts are rarely as intensely magnetized, but some samples - characterized by single domain magnetite formed from high temperature oxidation of olivine - approach this number.

  6. Morphology, Structure, and Origin of Island Paterae on Io

    NASA Astrophysics Data System (ADS)

    Howell, R. R.; Lopes, R. M.

    2011-12-01

    We are investigating both the small and large scale morphology of those paterae on Jupiter's moon Io which show central islands. At small scales a variety of features may be evidence of volatile transport processes. For example Loki Patera contains small bright spots colloquially known as sulfur bergs, which we suspect are fumarole deposits. They are near the limit of the best spatial resolution obtained in Voyager I images. Our preliminary results indicate their reflectance is consistent with sulfur (but not sulfur dioxide) as would be expected based on the temperatures seen in the infrared. At large scales we are beginning to model the stress patterns which could produce the overall morphology of island paterae. As discussed by Radebaugh (Ph.D. Dissertation, 2005) and Black (M.S. thesis, 2007), of 428 cataloged patera on Io, 35 contain bright islands. Most of these islands are irregularly shaped and may simply be regions not yet covered by lava. However several paterae, in particular Loki and Tupan, show more regular structure. Both patera have one straight edge, and in the case of Loki the most volcanically active part of the patera is located near that edge. As Turtle et al. (2001 JGR 106: 33175) and others have suggested, those straight edges may be faults which relieve the expected global compressive stresses and also act as magma conduits. Radebaugh (2005) has suggested that some of these large islands might be analogs of resurgent domes. We are investigating whether a hybrid stress model may be able to explain the overall morphology.

  7. NIMS Observes Increased Activity at Loki Patera, Io

    NASA Technical Reports Server (NTRS)

    1997-01-01

    Loki Patera, historically the most active and persistent hot spot on Io, is located on the hemisphere of Io always facing Jupiter. Loki Patera was the site of two plumes during the Voyager encounters, which were not seen during the early orbits of Galileo. Ground-based observers reported Loki Patera to be unusually dim during this time, marking a period of low volcanic activity.

    On 21 February 1997, during Galileo's sixth orbit, the Near Infrared Mapping Spectrometer (NIMS) on the Galileo spacecraft observed Io in daylight from a range of approximately 703,000 km (440,000 miles). The image on the left shows Io at a wavelength of 2.95 microns. Loki Patera is seen to be relatively quiescent (at longer wavelengths which are more sensitive to thermal emission, Loki Patera is more noticeable).

    A few weeks later, on March 12th 1997, ground based observers using the Infra-Red Telescope Facility (IRTF) on Mauna Kea, Hawaii, observed an intense brightening in the Loki region, so much that Loki was contributing 75% of Io's in-eclipse flux for this hemisphere. A large eruption was taking place! Other ground-based observations through March, April and May tracked the course of the activity and confirmed its location at Loki Patera.

    On 4 April 1997, NIMS again observed Io during the seventh orbit from a range of 556,000 km (348,000 miles), with Loki Patera positioned in darkness, close to the limb. The image on the right shows the increase in activity at Loki Patera, again at 2.95 microns. A preliminary single temperature fit to NIMS orbit seven Loki Patera hot spot data yields a temperature of 500 K and an area of over 800 square kilometers. That the image is so bright at this wavelength is an indication of the areal extent of the activity. It is also probable that some part of the volcanic material being erupted or exposed is at considerably higher temperatures than that of the 500 K single-temperature fit.

    Io is under observation by ground-based observers under

  8. Composition and location of volatiles at Loki Patera, Io

    NASA Astrophysics Data System (ADS)

    Howell, Robert R.; Landis, Claire E.; Lopes, Rosaly M. C.

    2014-02-01

    Volatiles play a critical role in determining the nature of volcanic activity on Earth, but their role in the volcanism on Io is less clear. To help determine that role we analyze Voyager and Galileo images of Loki Patera. Loki is the largest caldera in the Solar System and Io’s most powerful volcano, however its eruptive behavior is still not understood. It appears to be relatively volatile poor, in comparison to other sites like Pele where volatiles drive a 350 km high plume. A resurfacing wave, either from spreading flows or from foundering of a lava lake crust, periodically sweeps around Loki Patera. Photometry from Voyager I and II violet and blue images shows that most of the features in and around Loki have colors well matched by macroscopic mixing of sulfur and basalt. The dark western portion of the patera has the color of bare basalt. Assuming such a macroscopic sulfur-basalt mix, in the Voyager I images most of the rest of the patera appears to be covered with a background of 13-38% sulfur. We infer this background sulfur was deposited from the nearby plume observed by Voyager I and II. The surface of the patera is also dotted by numerous small bright areas which have colloquially been called “bergs”. We find that they are also composed of sulfur, with coverage ranging up to 100%. Darker regions adjacent to the patera, such as the “southwest overflow”, are a mixture of intermediate amounts of sulfur and basalt. The “bathtub ring” at the edge of the overflow is again roughly 100% sulfur, perhaps with significant amounts of SO2 included. Colors seen during the Voyager II flyby are also consistent with this general pattern, but most of the patera has a sulfur abundance higher than that seen in Voyager I, while the then-dark southern portion is again close to the reflectance of bare basalt. We have also analyzed the spatial distribution of the bergs. They clearly avoid the inner and outer margins of the patera, and they also avoid each other

  9. An Impact Genesis for Loki Patera?

    NASA Technical Reports Server (NTRS)

    Thorsos, I. E.; Davies, A. G.

    2005-01-01

    What happens when a large impact event takes place on a satellite with a thin crust and lithosphere? In the early Solar System impact cratering and volcanism were the dominate processes shaping the surfaces of the terrestrial planets. Impact events may have triggered additional volcanism by uplifting partially molten mantle material to the surface, where it melts due to pressure release. Subsequently, the shattered crust may have provided pathways for magma to reach the surface creating a longer term hot spot. As the crusts of the terrestrial planets thickened, the ability of impacts to trigger volcanism diminished [1]. However, the highly-volcanic jovian satellite Io is located in a "high-impact" area of the Solar System [2], a victim of material attracted by Jupiter s gravitational field. In 1994 huge impacts were observed when fragments of comet Shoemaker- Levy 9 impacted Jupiter. The large icy satellites of Jupiter (Europa, Ganymede and Callisto) are pockmarked with many impact craters. Yet no impact features have been found on Io [3]. This is because of rapid resurfacing of Io due to volcanism, estimated at approx.1 cm/year [4] which over short geological time erases evidence of impacts. Io, however, has a lithosphere over a molten or partially-molten mantle [e.g., 5], and the effects of a sufficiently large impact may extend far beyond the evolution of the impact crater alone. At least one example of impact-triggered volcanism may exist in the Solar System today: the Loki Patera complex on Io.

  10. Ionian Paterae: New Insights from Observations, Numerical Modeling and Laboratory Simulations

    NASA Astrophysics Data System (ADS)

    Gregg, T. K.; Lopes, R. M.; Black, S. M.; Lougen, J.

    2006-12-01

    To constrain the behavior of Ionian volcanic paterae in general, and Loki Patera in particular, we have used the following techniques in concert: 1) geologic mapping and analyses; 2) laboratory simulations; and 3) mathematical modeling. Here, we present preliminary results from the synthesis of these data. Loki Patera (310°W, 12°°N) is significantly different from the rest of the Ionian paterae for the following reasons: 1) its surface area falls 6 s outside the range for other Ionian paterae; 2) it is the only patera containing a bright "island" that is cut by dark lineaments; 3) at times of a thermal brightening event, it emits up to 15% of Io's global heat flux. Debate continues over whether Loki Paterae is an overturning lava lake, or a depression whose floor is periodically resurfaced by lava flows. Laboratory simulations, in which corn syrup or polyethylene glycol wax (PEG) were extruded into a square tank through 1 or 2 floor vents at a constant rate, were conducted to provide insight into Loki Patera's behavior. Results from both sets of experiments suggest that a single convection cell would be difficult to establish at Loki Patera. Crustal foundering of a lava lake may be possible under special conditions. Given the unique nature of Loki Patera and its island, we propose that the island may be similar to a resurgent dome in a terrestrial caldera complex composed primarily of evolved lavas, such as Long Valley Caldera, California. We examined other paterae that contain bright "islands" on their floors in an effort to constrain their origins. Geologic mapping, and shape analyses of the paterae and the islands they contain, suggest that most paterae islands are patches of cooled lava on the paterae floor. Only about 8% of paterae islands have morphologies and geologic relations that are consistent with a tectonic origin.

  11. Seeking Signs of Life in Nili Patera with Icelandic Sinter Field Exploration.

    NASA Astrophysics Data System (ADS)

    Skok, J. R.; Farmer, J. D.; Parente, M.; Gaskin, J.; Kaasalainen, H.; Tobler, D.; Jerman, G.

    2015-12-01

    The past decade of Martian orbital and surface exploration has made it clear that the planet could have supported life as we know it in many places throughout much of it's history. The next step in exploration will be to find the evidence for and characterize any preserved Martian life. The jump from confirming habitability to finding life will be difficult and likely require a systemic surface exploration of multiple, specific sites. One site, the sinter mounds of the Nili Patera caldera, provides the ideal combination of hot, neutral to alkaline waters that can develop or support life and the sinter precipitation to preserve it. Nili Patera also provides deposits that are well mapped from orbit allowing a mission to pinpoint the target rocks. With this target known, we can develop the mission, the payload and the science to fit the goals. Several sinter field sites in Iceland were selected for mission testing. They were selected to provide diversity in scale, chemistry and complexity. At each site, we asked the same questions that would drive a mission to Mars. Was there life? What are its preserved properties? What are the environmental history of the sinters and the volcanic history of the local terrain? These questions were investigated with spectral, compositional and morphological analysis. By investigating these questions in Iceland, we will determine which observations, in terms of terrain access and instrument selection are required for mission success on Mars. We report the results from the August 2015 expedition, the first of two planned field seasons. This summer was focused on finalizing the field locations, acquiring mapping data and an initial sampling campaign to determine expected composition and calibrate instruments for year two. With this information, we will determine an investigation plan consistent with a range of mission types from robotic lander to sample return to human exploration. We will also determine the instruments required by the

  12. Loki Patera as the Surface of a Magma Sea

    NASA Technical Reports Server (NTRS)

    Matson, D. L.; Davies, A. G.; Veeder, G. J.; Rathbun, J. A.; Johnson, T. V.

    2004-01-01

    Inspired by the finding of Schubert et al that Io's figure is consistent with a hydrostatic shape, we explore the consequences of modeling Loki Patera as the surface of a large magma sea. This model is attractive because of its sheer simplicity and its usefulness in interpreting and predicting observations. Here, we report on that work.

  13. Mars

    NASA Technical Reports Server (NTRS)

    McKay, Christopher P.; Cuzzi, Jeffrey N. (Technical Monitor)

    1995-01-01

    There is direct geomorphological evidence that in the past Mars had large amounts of liquid water on its surface. Atmospheric models would suggest that this early period of hydrological activity was associated with the presence of a thick atmosphere and warmer temperatures. It is possible that at some time in the future we might recreate a habitable climate on Mars, returning it to the life-bearing state it may have enjoyed early in its history. Our studies of Mars are still in a preliminary state but everything we have learned suggests that it may be possible to restore Mars to a habitable climate. Mars' current scientific value is indisputable but it is certainly true that extensive exploration followed by a careful and studied program of introducing life would yield an even greater scientific harvest. The scientific knowledge gained by studying the ways in which a biosphere could be introduced on Mars may inform us as to the preservation of the one on Earth.

  14. A stochastic basis to the spatially uniform distribution of randomly generated Ionian paterae

    NASA Astrophysics Data System (ADS)

    Shoji, D.; Hussmann, H.

    2016-10-01

    Due to its tidally heated interior, Io is a geologically very active satellite that bears many volcanic features. It is observed that the mean nearest neighbor distance of each volcanic feature, called a patera, is larger than that of a random distribution, which implies that the spatial distribution of paterae is uniform rather than random. However, it is uncertain how the paterae are organized into a uniform distribution. We suggest the mechanism of Io's uniformly distributed paterae considering localized obliteration of old features. Instead of geological modeling, we performed stochastic simulations and statistical analyses for the obliteration of quiescent paterae. Monte Carlo calculations with Gaussian obliteration probability show that if the width of obliteration probability is approximately 80 km and the volcanic generation rate is ˜5.0 × 10-6 km-2 Ma-1, uniform distribution and the observed number density of paterae are attained at the 2σ level on a time scale of approximately 6 Myr. With this generation rate and width of the obliteration probability, the averaged distance of one patera to the nearest patera (mean nearest neighbor distance) is approximately 200 km, which is consistent with the observed value. The uniformity of the distribution is maintained once it is achieved. On regional scales, Io's paterae would naturally evolve from random into uniform distributions by the obliteration of old and quiescent features.

  15. Cleopatra Patera on Venus: Venera 15/16 evidence for a volcanic origin.

    USGS Publications Warehouse

    Schaber, G.G.; Kozak, R.C.; Masursky, H.

    1987-01-01

    The non-concentric nature, anomalous depth, and terraced morphology of the nested craters that compose Cleopatra Patera are more closely analogous to volcanic craters (calderas) than multi-ring impact structures. Associated deposits northeast and downslope of the Patera first recognized on Venera 15/16 radar images are interpreted as volcanic plains related to, and perhaps cogenetic with, Cleopatra. A volcanic origin not only is easily reconciled with the tectonic setting of the Patera, it is almost required by the correlation between the Patera and regional structural trend. -from Authors

  16. Geologic map of the Sappho Patera Quadrangle (V-20), Venus

    USGS Publications Warehouse

    McGill, George E.

    2000-01-01

    The Sappho Patera quadrangle (V–20) of Venus is bounded by 0° and 30° East longitude, 0° and 25° North latitude. It is one of 62 quadrangles covering the entire planet at a scale of 1:5,000,000. The quadrangle derives its name from Sappho Patera, a large rimmed depression (diameter about 225 km) lying on top of a shield-shaped mountain named Irnini Mons. Sappho, a noted Greek poet born about 612 B.C., spent most of her life on the island of Lesbos. All of her works were burned in 1073 by order of ecclesiastical authorities in Rome and Constantinople. What little survives was discovered in 1897 as parts of papier mâché coffins in the Fayum (Durant, 1939). The Sappho Patera quadrangle includes the central portion of Eistla Regio, an elongated, moderately elevated (relief ~1 km) region extending for about 7,500 km west-northwestward from the west end of Aphrodite Terra. It is generally interpreted to be the surface manifestation of one or more mantle plumes (Phillips and Malin, 1983; Stofan and Saunders, 1990; Kiefer and Hager, 1991; Senske and others, 1992; Grimm and Phillips, 1992; Solomon and others, 1992). Eistla Regio is dominated by several large volcanic features. All or parts of four of these occur within the Sappho Patera quadrangle: the eastern flank of Gula Mons, Irnini Mons, Anala Mons, and Kali Mons. The quadrangle also includes eight named coronae: Nehalennia, Sunrta, Libera, Belet-Ili, Gaia, Asomama, Rabzhima, and Changko. A major rift extends from Gula Mons in the northwestern corner of the quadrangle to Libera Corona near the east border. East of Irnini and Anala Montes this rift is named Guor Linea; west of the montes it is named Virtus Linea. In addition to these major features, the Sappho Patera quadrangle includes numerous smaller volcanic flows and constructs, several unnamed coronae and corona-like features, a complex array of faults, fractures, and wrinkle ridges, and extensive plains that are continuous with the regional plains that

  17. Martian Hot Springs? Silica deposits in the Nili Patera Caldera.

    NASA Astrophysics Data System (ADS)

    Skok, J. R.; Mustard, J. F.; Ehlmann, B. L.; Murchie, S. L.

    2011-12-01

    detected just west of the cone center near it's apex and appears to be exposed outcrop. The remaining detections are quasi-circular mounds on the caldera floor. One isolated large deposit is at the southern edge of the cone while the majority of deposits are in an 8,000 km2 field directly southwest of the cone that contains dozens of deposits of varying sizes. Recently confirmed deposits are also located in the far field, 10 km to the southwest of the cone but still confined to the dacite lava flow. These show that the deposits are more widespread than the immediate vicinity of the volcanic cone. This volcanically driven hydrothermal system and the resulting hot spring environments on Mars has significance for our understanding of Martian volcanic systems and for the search for habitability. Terrestrial hot springs are known to be ideal locations for microbial activity and for the sequestration and long-term preservation of biosignatures . Hot spring silica sinter deposits are among the best materials for preserving signs of habitability making the Nili Patera deposits an ideal location for future focused study.

  18. Paterae on Io: Volcanic Activity Observed by Galileo's NIMS and SSI

    NASA Technical Reports Server (NTRS)

    Lopes, Rosaly; Kamp, Lucas; Smythe, W. D.; Carlson, R.; Radebaugh, Jani; Gregg, Tracy K.

    2003-01-01

    Paterae are the most ubiquitous volcanic construct on Io s surface. Paterae are irregular craters, or complex craters with scalloped edges, interpreted as calderas or pit craters. Data from Galileo has shown that the activity of Ionian paterae is often confined to its interior and that generally lava flows are not seen spilling out over the edges. We use observations from Galileo s Near-Infrared Mapping Spectrometer (NIMS) to study the thermal emission from several Ionian paterae and compare them with images in visible wavelengths obtained by Galileo s Solid State Imaging System (SSI). Galileo s close fly-bys of Io from 1999 to 2001 have allowed NIMS to image the paterae at high spatial resolution (1-30 km pixel). At these scales, several of these features reveal greater thermal emission around the edges, which can be explained as the crust of a lava lake breaking up against the paterae walls. Comparisons with imaging data show that lower albedo areas (which are indicative of young lavas) coincide with higher thermal emission areas on NIMS data. Other paterae, however, show thermal emission and features in the visible that are more consistent with lava flows over a solid patera floor. Identifying eruption styles on Io is important for constraining eruption and interior models on Io.

  19. Interpretation of collapsed terrain on Mars

    NASA Astrophysics Data System (ADS)

    Ewa Zalewska, Natalia; Skocki, Krzysztof

    2016-10-01

    On the images from HiRISE camera within volcanoes and circumpolar areas there are depressions that can be explained in two ways, either by melting subsurface layer of ice or by cooling of lava which forms branch intrusion and flank craters underneath. On many pictures from Mars similar cavities are found on the slopes of Martian craters on Arsia Mons , Pavonis Mons on northern hemisphere and Alba Patera on southern hemisphere. Such cavities can be compared to a Hawaiian type volcanoes. At the top of Mauna Loa linearly arranged craters can be seen, strikingly similar to those on Arsia Mons . Basing on map ice content measured by Odyssey GRS apparatus, in this place of the volcanic cone, quite small ice content can be observed that varies in the range of 2-4% hydrogen abundance. It is therefore difficult to explain these collapses by unfreezing of subsurface ice. In an infrared spectrum of these areas there are no bands of water in the CRISM spectra, although it does not say that the water in the form of ice couldn't have been there before. In the central part of Chryse, there are series of chains depressions caused most likely by the collapse of land. These forms have been associated with an open pingo type system additionally with assisted topography of the area or tectonics and internal cracks in the rocks. These are noticed on the slopes of craters or wherever the area decline. Then flowing subsurface water or brine coming from the ice layer could while freezing accumulate and create a longitudinal hill that collapsed due to seasonal thawing forming gullies or canyons . At the end of these gullies remaining trace of the leak can be seen, as if there was a crack in the ground and liquid flew out on the surface. Cryosubsurface processes on Mars can support the hypothesis of geochemical origin of water, which separates from the magma, and its primary source comes from the protoplanetary disk. The water separated from the magma migrates up to the surface and if the

  20. The Western Hesperia Planum Region of Mars: MGS-based Revelations

    NASA Astrophysics Data System (ADS)

    Gregg, T. K.; Sakimoto, S. E.; Crown, D. A.; Meyer, B. R.; Gittings, H.

    2001-12-01

    Tyrrhena Patera ( ~22° S, 252° W), Mars, is located on the western edge of Hesperia Planum and ~2500 km NW of the Hellas basin. The volcano's flanks are dissected by broad (>6 km) flat-floored radial valleys; valley morphology is consistent with modification by groundwater sapping processes. Based on morphology and surface texture as observed in Mars Observer Camera (MOC) and Viking Orbiter (VO) images, the shield materials appear to be comprised of fine-grained, friable material that have been interpreted to be pyroclastic deposits. A large (~1000 km x 200 km) lava flow field extends from the summit caldera complex to the southwest. The flow field is younger than adjacent Hesperia Planum, and crosscuts Tyrrhena Patera shield materials, indicating that Tyrrhena Patera experienced a transition from early explosive to later effusive volcanism. Using datasets obtained by Mars Global Surveyor (MGS), we have learned that the western Hesperia Planum region is more complex and contains more volcanic deposits than previously thought. Tyrrhena Patera deposits, identified using MOC and the Mars Observer Laser Altimeter (MOLA) data, extend more than 500 km to the west of the summit caldera complex and more than 550 km to the northwest. This observation increases the area covered by Tyrrhena Patera shield materials by a factor of four and suggests that the deposits are pyroclastic flows rather than falls, and that these flows were highly mobile. Such an inference is consistent with a "wet" Mars at the time of these eruptions. MOC and MOLA data further reveal cycles of deposition and erosion, which suggests that explosive activity at Tyrrhena Patera may have continued into the Hesperian Epoch. Finally, MOLA investigations of the lava flow field associated with Tyrrhena Patera have revealed that the individual flow lobes have fundamentally different morphologies from those found at shield volcanoes in the northern hemisphere.

  1. 3D morphometry of valley networks on Mars from HRSC/MEX DEMs: Implications for climatic evolution through time

    NASA Astrophysics Data System (ADS)

    Ansan, V.; Mangold, N.

    2013-09-01

    valley networks have been identified mainly in the Noachian heavily cratered uplands. Eight dense branching valley networks were studied in Noachian terrains of Huygens, Newcomb and Kepler craters, south Tyrrhena Terra, and Thaumasia, in Hesperian terrains of Echus Plateau and west Eberswalde craters, and in Amazonian terrains of Alba Patera, using images and digital elevation models from the Mars Express High Resolution Stereo Camera to determine 2D and 3D morphometric parameters. Extracted geomorphic parameters show similar geometry to terrestrial valleys: drainage densities, organization from bifurcation ratios and lengths ratios, Hack exponent consistent with terrestrial values of ~0.6, and progressive deepening of valleys with increasing Strahler order. In addition, statistics on valley depths indicate a deeper incision of Noachian valleys compared to younger post-Noachian valleys (<25 m for Amazonian ones compared to >100 m for Noachian ones), showing a strong difference in fluvial erosion. These characteristics show that dense Martian valley networks formed by overland flows in relation to a global atmospheric water cycle in Noachian epoch and confirm that the later stages of activity may be related to shorter duration of activity, distinct climatic conditions, and/or regional processes, or conditions.

  2. Cleopatra Patera on Venus - Venera 15/16 evidence for a volcanic origin

    NASA Astrophysics Data System (ADS)

    Schaber, G. G.; Kozak, R. C.; Masursky, H.

    1987-01-01

    The nonconcentric nature, anomalous depth, and terraced morphology of the nested craters that compose Cleopatra Patera are more closely analogous to volcanic craters (calderas) than multiring impact structures. Associated deposits northeast and downslope of the Patera first recognized on Venera 15/16 radar images are interpreted as volcanic plains related to, and perhaps cogenetic with, Cleopatra. The plains lavas probably originated as effusions from a radial rift zone or ring fissures. Rim deposits surrounding Cleopatra are asymmetric along the structural fabric of the region, also indicating fissure-type eruptions. Finally, a volcanic origin not only is easily reconciled with the tectonic setting of the Patera, it is almost required by the correlation between the Patera and regional structural trend.

  3. Geology and Topography of Ra Patera, Io, in the Voyager era: Prelude to Eruption

    NASA Technical Reports Server (NTRS)

    Schenk, Paul M.; McEwen, Alfred; Davies, A. G.; Davenport, Trevor; Jones, Kevin; Fessler, Brian

    1997-01-01

    Voyager era stereo images are used to map the geology and topography of Ra Patera (a major active volcanic center and possible site of sulfur eruptions on Io). The summit of Ra Patera reaches only approx.1 km above the surrounding plains. Pre-Voyager-era lava flows occur on slopes of 0.1-0.3 deg, comparable to the lunar mare. These flows were emplaced at either low viscosities, high eruption rates, or both. A 600- km-long ridged mountain unit (rising to approx. 8 km near Carancho Patera) forms a 60 by 90 km wide plateau approx. 0.5 km high 50 km east of Ra Patera. The new lava flows observed by Galileo flowed around the southern edge of this plateau.

  4. Heterogeneities in the thickness of the elastic lithosphere of Mars: Constraints on heat flow and internal dynamics

    SciTech Connect

    Solomon, S.C. ); Head, J.W. )

    1990-07-10

    Derived values of the thickness of the effective elastic lithosphere on Mars are converted to estimates of lithospheric thermal gradients and surface heat flow by finding the thickness of the elastic-plastic plate having the same bending moment and curvature, subject to assumed strain rates and temperature-dependent flow laws for crustal and mantle material. Local thermal gradients and heat flow values so estimated were 10-14 K km{sup {minus}1} and 25-35 mW m{sup {minus}2}, respectively, at the time of formation of flexurally induced graben surrounding the Tharsis Montes and Alba Patera, while gradients and heat flow values of less than 5-6 K km{sup {minus}1} and 17-24 mW m{sup {minus}2}, respectively, characterized the lithosphere beneath the Isidis mascon and Olympus Mons at the time of emplacement of these loads. On the basis of the mean global thickness of the elastic lithosphere inferred to support the Tharsis rise and estimates of mantle heat production obtained from SNC meteorites, it is suggested that the present average global heat flux on Mars is in the range 15-25 mW m{sup {minus}2}. Approximately 3-5% of this heat flux during the Amazonian epoch has been contributed by excess conducted heat in the central regions of major volcanic provinces. Most likely, this excess heat flux has been delivered to the base of the lithosphere by mantle plumes. The fractional mantle heat transport contributed by plumes during the last 2 b.y. on Mars is therefore similar to that at present on Earth.

  5. Composition and spatial distribution of volatile deposits in Loki Patera, Io

    NASA Astrophysics Data System (ADS)

    Landis, Claire E.

    Loki Patera is an active volcanic feature on Jupiter's moon Io which, at approximately 200 km in diameter, is perhaps the largest active lava lake in the solar system. Several images taken by the narrow angle camera of Voyager 1 during its 1979 flyby of Io reveal the patera surface is populated with many bright features roughly 2 to 4 km in diameter, colloquially referred to as "bergs." The bergs may be gas vents, similar to terrestrial fumaroles, which allow the sulfur-rich volatiles in the lava beneath the solid patera crust to escape and deposit on the surface. This thesis examines the spatial distribution of the bergs and their spectral signature in comparison with other features in the Loki region. The spectral analysis specifically focuses on the brightness in the blue and violet filters in an attempt to determine their composition and better understand how the bergs are related to the volcanic activity observed at Loki. The spatial distribution analysis reveals that the bergs are not randomly distributed across the patera surface and they avoid the inner and outer margins of the patera. There are no bergs within 4.96 km of the outer margin and only one berg occurs closer than 4.02 km to the inner margin. The bergs also avoid each other; bergs are on average 5.34 km from each other, and there is little deviation from this mean aside from the bergs in the southwest corner, which are spaced further apart. This corner has fewer bergs than elsewhere in the patera and is the site of the most volcanic activity. Data from the Voyager and Galileo missions were included in the spectral analyses. Assuming a macroscopic mixture, the spectral signature of the bergs indicate compositions ranging from bare basalt in the southwestern portion of the patera to approximately 43% sulfur and 57% basalt for the bergs. Other features around Loki, such as the large island in the middle of the patera, have slightly different brightnesses in the blue and violet filters which may

  6. Topography of closed depressions, scarps, and grabens in the North Tharsis region of Mars: implications for shallow crustal discontinuities and graben formation

    USGS Publications Warehouse

    Davis, Philip A.; Tanaka, Kenneth L.; Golombek, Matthew P.

    1995-01-01

    Using Viking Orbiter images, detailed photoclinometric profiles were obtained across 10 irregular depressions, 32 fretted fractures, 49 troughs and pits, 124 solitary scarps, and 370 simple grabens in the north Tharsis region of Mars. These data allow inferences to be made on the shallow crustal structure of this region. The frequency modes of measured scarp heights correspond with previous general thickness estimates of the heavily cratered and ridged plains units. The depths of the flat-floored irregular depressions (55-175 m), fretted fractures (85-890 m), and troughs and pits (60-1620 m) are also similar to scarp heights (thicknesses) of the geologic units in which these depressions occur, which suggests that the depths of these flat-floored features were controlled by erosional base levels created by lithologic contacts. Although the features have a similar age, both their depths and their observed local structural control increase in the order listed above, which suggests that the more advanced stages of associated fracturing facilitated the development of these depressions by increasing permeability. If a ground-ice zone is a factor in development of these features, as has been suggested, our observation that the depths of these features decrease with increasing latitude suggests that either the thickness of the ground-ice zone does not increase poleward or the depths of the depressions were controlled by the top of the ground-ice zone whose depth may decrease with latitude. Deeper discontinuities are inferred from fault-intersection depths of 370 simple grabens (assuming 60° dipping faults that initiate at a mechanical discontinuity) in Tempe Terra and Alba Patera and from the depths of the large, flat-floored troughs in Tempe Terra. The frequency distributions of these fault-intersection and large trough depths show a concentration at 1.0-1.6 km depth, similar to data obtained for Syria, Sinai, and Lunae Plana. The consistency of these depth data over

  7. Spectral and Spatial Analysis of Volatile Deposits in Io's Loki Patera

    NASA Astrophysics Data System (ADS)

    Landis, C. E.; Howell, R. R.

    2012-12-01

    Loki Patera is an active volcanic feature approximately 200 km in diameter on Jupiter's moon Io. The goals of this research are to better understand the nature of volatile distribution in and around the Loki region. Images taken by Voyager I show a number of bright features distributed across the patera surface. These features, referred to as "bergs," may be fumaroles which allow sulfur gases from the lava beneath the hardened crust to escape onto the surface. By examining the spatial distribution of the bergs and the spectral signatures of bergs and other features around Loki Patera, we can better understand their role in the volcanic activity observed at Loki, and perhaps elsewhere on Io. Spectral data from the Voyager and Galileo missions were examined using ISIS3, a program suite developed by the USGS. Photometric corrections were applied to the images to adjust for changes in lighting geometry. The spatial distribution of the bergs was examined using ArcMap. Initial results indicate that the bergs seldom occur near the inner and outer edges of the patera, which are known to be hotter than other parts of the patera. The lack of bergs in this area suggests that thermal properties of the crust may control the distribution of the bergs. The spacing of the bergs, which on average are about 6 km from each other, and other distribution statistics are used to test whether there is some maximum area of crust in which one berg can accommodate the escaping gases. The spectral signatures of the bergs themselves are compared to other surface features in and around the patera. Further study of the bergs and other features will continue to shed light on the underlying geologic and volcanic processes responsible for the activity at Loki. This work was supported in part by NASA JDAP grant NNX09AE06G.

  8. Changes near the Volcano Loki Patera on Io

    NASA Technical Reports Server (NTRS)

    1996-01-01

    Four views of the volcano Loki Patera on Jupiter's moon Io showing changes seen on June 27th, 1996 by the Galileo spacecraft as compared to views seen by the Voyager spacecraft during the 1979 flybys. Clockwise from upper left is a Voyager 1 high resolution image, a Voyager 1 color image, a Galileo color image, and a Voyager 2 color image. North is to the top of the picture. During the Voyager flybys large dense volcanic plumes erupting from each end of the dark linear 'fissure' to the northeast of the dark caldera and plume deposits obscured much of the surrounding surface. These dark jets are not visible in the Galileo image, and other images have confirmed that the Loki plumes were inactive during this Galileo encounter. Ground-based observers have determined that the Loki hot spot, historically the most energetic on Io, has been unusually dim. The fissure appears extended and elongated to the east and southwest, perhaps also resulting in a migration of the plume vents. There is an enlarged dark spot to the west of Loki. The materials just south and northeast of the caldera appear more reddish color. Images are 894 km wide. The Jet Propulsion Laboratory, Pasadena, CA manages the mission for NASA's Office of Space Science, Washington, DC. This image and other images and data received from Galileo are posted on the World Wide Web, on the Galileo mission home page at URL http://galileo.jpl.nasa.gov. Background information and educational context for the images can be found at URL http://www.jpl.nasa.gov/galileo/sepo

  9. Explosive volcanic deposits on Mars: Preliminary investigations

    NASA Technical Reports Server (NTRS)

    Crown, D. A.; Leshin, L. A.; Greeley, Ronald

    1987-01-01

    Two investigations were undertaken to examine possible large scale explosive volcanic deposits on Mars. The first includes an analysis of Viking Infrared Thermal Mapper (IRTM) data covering the vast deposits in the Amazonis, Memnonia, and Aeolis regions. These postulated ignimbrites have been previously mapped, and at least five high resolution nighttime IRTM data tracks cross the deposits. Preliminary analysis of the data covering Amazonis Planitia show that local features have anomalous thermal inertias but the ignimbrites as a whole do not consistently have significantly different thermal inertias from their surroundings. Preliminary photogeologic and IRTM studies of the large and small highland paterae have also begun. The purpose of IRTM studies of postulated Martian explosive volcanic deposits is to determine the physical properties of the proposed ignimbrites. If volcanic deposits are exposed at the surface, high thermal inertias, as are observed for Apollinaris Patera, should be present.

  10. Time-Evolution and Thermal Mapping of Io's Loki Patera at High Resolution

    NASA Astrophysics Data System (ADS)

    de Kleer, Katherine R.; Skrutskie, Michael F.; Leisenring, Jarron; de Pater, Imke; Davies, Ashley; Conrad, Al; Caleb Resnick, Aaron; Hinz, Philip; Defrère, Denis; Veillet, Christian

    2016-10-01

    Observations of Loki Patera with Keck, Gemini N, and the Large Binocular Telescope have yielded a wealth of information in the past several years. Observations with adaptive optics at the Keck and Gemini N telescopes have captured multiple brightening events since 2009. High-cadence observations of the three most recent events place constraints on the thermal properties of the magma and indicate a dependency of the observed intensity on either viewing geometry or mean anomaly. Large Binocular Telescope Interferometer (LBTI) observations during a Europa mutual event have yielded the first-ever temperature map of the entire patera floor at high spatial resolution. M-band (4.7-micron) images were recorded during the event at a cadence of 123 milliseconds, corresponding to a spatial resolution of 10 km across the entire ~200-km patera. This represents a factor of 40 improvement over the spatial resolution achieved by standard adaptive optics imaging with a 10-m telescope at this wavelength. A map of the lava age distribution within the patera is derived from the temperature map using models for cooling basaltic lavas, and the resurfacing rate is calculated. This age distribution, as well as the locations of emission derived from the Keck and Gemini N observations, suggests that resurfacing proceeds in a clockwise direction, contrary to previous findings. All data are consistent with resurfacing by an overturn front on a magma sea, but other resurfacing mechanisms are not ruled out.

  11. Sulfur "Bergs" and Sulfur Pools: Loki and Tupan Patera on Io

    NASA Astrophysics Data System (ADS)

    Howell, R. R.; Lopes, R. M.; Landis, C. E.; Allen, D. R.

    2012-12-01

    Loki and Tupan Patera on Io show numerous features related to the presence of volatiles. There are both striking similarities and distinct differences in the way the volatiles have acted at these two sites. At Loki numerous small bright features, colloquially known as sulfur "bergs", are distributed across the dark patera surface. We map their spatial distribution and spectral properties (Landis et al., this conference) and model sulfur vapor transport processes (Allen et al. this conference) to determine if those bright features are consistent with sulfur fumarole deposits. Alternatively, the "bergs" may represent topographic highs (kipukas) left un-resurfaced by the recurrent activity at Loki. To test this we examine Voyager, Galileo, and New Horizons images to determine if any changes in their spatial distribution have occurred over the 1979 through 2007 period. We also discuss further a statistical analysis of their size and spectral reflectance. Tupan shows an overall morphology similar to Loki, with a central island and one straight margin. It also shows linear features extending across the island. However instead of the dark eastern portion of the patera containing a myriad of small bright features like the Loki "bergs" which avoid the margins, Tupan shows higher albedo deposits concentrated at the margins. And in the higher albedo western portion of Tupan Patera numerous low albedo features can be interpreted as dark silicates erupting or eating through a volatile rich crust. Unlike Loki, these intra-patera features at Tupan clearly have sharply defined edges, indicating surface flow processes rather than possible vapor effects. However both outside the main Tupan Patera walls and on the island there are more diffuse patterns consistent with vapor transport. A detailed comparison of reflectance at violet through very near infrared wavelengths helps elucidate these effects. As also found at Loki, a low violet reflectance indicates that sulfur is abundant on

  12. Geologic Map of the Thaumasia Region, Mars

    USGS Publications Warehouse

    Dohm, Janes M.; Tanaka, Kenneth L.; Hare, Trent M.

    2001-01-01

    ). The medium-resolution Viking images used for mapping and base preparation also formed the basis of the 1:2,000,000 scale subquadrangle series. Earlier geologic maps of all or parts of the region include: (1) maps of the Phoenicis Lacus, Coprates, Thaumasia, and Argyre quadrangles at 1:5,000,000 scale based mainly on Mariner 9 images (respectively, Masursky and others, 1978; McCauley, 1978; McGill, 1978; and Hodges, 1980), (2) the global map of Mars at 1:25,000,000 (Scott and Carr, 1978) compiled largely from the 1:5,000,000 scale geologic maps, (3) maps showing lava flows in the Tharsis region at 1:2,000,000 scale compiled from Viking and Mariner 9 images (Scott, 1981; Scott and Tanaka, 1981a, b; Scott and others, 1981), (4) the map of the western equatorial region of Mars at 1:15,000,000 scale based on Viking images (Scott and Tanaka, 1986), and (5) the map of the Valles Marineris region at 1:2,000,000 scale compiled from Viking images (Witbeck and others, 1991). The previous maps have described the overall geology and geomorphology of the region but have not unraveled the detailed stratigraphy and complex evolution of this unique and geologically diverse martian province. The main purpose of this comprehensive mapping project is to reconstruct the stratigraphic, structural, and erosional histories of the Thaumasia region. The region is the last major province of the Tharsis region to undergo detailed structural mapping using Viking images; its history is essential to documenting the overall tectonic history of Tharsis. Other provinces of Tharsis that have been structurally mapped include Syria Planum (Tanaka and Davis, 1988), Tempe Terra and Ulysses Patera (Scott and Dohm, 1990b), and Alba Patera (Tanaka, 1990). Another primary mapping objective is to determine the region's volcanic history and assess the relations among fault systems and volcanoes (Wise and others, 1979; Scott and Tanaka, 1980; Whitford-Stark, 1982; Scott and Dohm, 1990a). A secondary mapping

  13. "Active" and "Passive" Lava Resurfacing Processes on Io: A Comparative Study of Loki Patera and Prometheus

    NASA Technical Reports Server (NTRS)

    Davies, A. G.; Matson, D. L.; Leone, G.; Wilson, L.; Keszthelyi, L. P.

    2004-01-01

    Studies of Galileo Near Infrared Mapping Spectrometer (NIMS) data and ground based data of volcanism at Prometheus and Loki Patera on Io reveal very different mechanisms of lava emplacement at these two volcanoes. Data analyses show that the periodic nature of Loki Patera s volcanism from 1990 to 2001 is strong evidence that Loki s resurfacing over this period resulted from the foundering of a crust on a lava lake. This process is designated passive , as there is no reliance on sub-surface processes: the foundering of the crust is inevitable. Prometheus, on the other hand, displays an episodicity in its activity which we designate active . Like Kilauea, a close analog, Prometheus s effusive volcanism is dominated by pulses of magma through the nearsurface plumbing system. Each system affords views of lava resurfacing processes through modelling.

  14. Geology of the Uranius Group Volcanic Constructs: Uranius Patera, Ceraunius Tholus, and Uranius Tholus

    USGS Publications Warehouse

    Plescia, J.B.

    2000-01-01

    Uranius Patera, Ceraunius Tholus, and Uranius Tholus (three small constructs in the northeast Tharsis region) date to the Late Hesperian Epoch and define the earliest phases of constructional volcanism in the Tharsis province. All three volcanoes are interpreted as shields, built by effusive eruptions of low-viscosity lavas, presumably basalt. Ceraunius Tholus and Uranius Tholus also record pyroclastic volcanism in the form of mantling deposits on their flanks; Uranius Patera either did not experience pyroclastic volcanism or the deposits were subsequently buried by later effusive eruptions. Troughs observed on the flanks of Ceraunius Tholus and Uranius Tholus are interpreted to have been formed by fluvial surface runoff. These constructs are coeval with other small edifices in western Tharsis province and are coeval with plains volcanism in the southern Tharsis, Syria, and Sinai regions. ?? 2000 Academic Press.

  15. Global Near-IR Maps of Io from Gemini-N and Keck Observations in 2010, with a Specific Emphasis on Kanehekili Fluctus, Janus Patera, and Loki Patera

    NASA Astrophysics Data System (ADS)

    De Pater, I.; Davies, A. G.; Adamkovics, M.; McGregor, A.; Observing Team, G.

    2013-12-01

    We have constructed global maps of Io from observations obtained at 1-5 μm in 2010 using the adaptive optics systems on the Keck and Gemini telescopes. We compare these maps with those obtained in 2001 [1]. Although the total emission from all hot spots combined at each wavelength is similar for the two years, the spatial brightness distribution is very different, a reflection of evolving style and magnitude of volcanic activity. In 2010 thermal emission in the near-infrared was dominated by Loki Patera and Kanehekili Fluctus. We also present new timelines of thermal emission from Kanehekili Fluctus and Loki and Janus Paterae, updating timelines in recent publications [2, 3] with additional Keck adaptive optics data obtained between 2003 and 2010. These new timelines are the most comprehensive plots ever produced of the volcanic thermal emission variability for these or any other locations on Io, utilizing data from multiple ground- and space-based assets. The timeline plot shows that in 2010 Kanehekili Fluctus (as seen by Gemini) was briefly exceptionally brighter than ever seen before, evidence of a short-lived but highly-energetic eruption episode. Acknowledgements: AGD is supported by a grant from the NASA OPR Program. References: [1] Marchis et al. (2005) Icarus, 176, 96-122. [2] Davies et al. (2012) Icarus, 221, 466-470. [3] Rathbun and Spencer (2010) Icarus, 209, 625-630.

  16. Lithospheric Structure and Patera Formation on Io: Implications for Future Observations

    NASA Astrophysics Data System (ADS)

    Jaeger, W. L.; Davies, A. G.

    2008-12-01

    On Jupiter's moon Io, the interaction between volcanism and tectonism is strongly modulated by the structure of the lithosphere. Previous work has shown that Io's prodigious volcanism leads to the rapid burial of its surface and, consequently, the global subsidence of the materials that compose its lithosphere. This, in turn, generates large horizontal compressive stresses, which drive the thick-skinned thrust faulting that uplifts Io's mountains. Because horizontal compression is an ongoing process that proceeds ever more rapidly with increasing depth, we assume in our model that the lithosphere is pervasively fractured and its stress state is governed by frictional sliding. The result is that pore space within the crust disappears rapidly with depth, and SO2 (which is the dominant volatile species and which melts at a relatively low pressure) is confined to the near-surface region. Thus, Io's lithosphere is compositionally stratified, with a low-density SO2-dominated layer up to a few kilometers thick overlying a denser mafic or ultramafic silicate layer a few tens of kilometers thick. Rising magma should achieve neutral buoyancy near the interface between these two layers, and if that interface is abrupt, the magma may spread laterally there for purely mechanical reasons as well. The heat from these shallow sill-like intrusions is expected to mobilize the overlying volatiles, eventually unroofing the sill or lava lake. The overburden can be removed both by the melting and lateral flow of the volatiles and by their sublimation. (SO2 atop warm silicate lavas is predicted to sublimate at a rate of ~100 m/yr.) Hence, ionian paterae may be more analogous to the depressions formed in ice during terrestrial subglacial eruptions than to true volcanic calderas. These models for Io's lithospheric structure and its patera formation should be tested by future spacecraft missions. Three observations that would be particularly useful are (a) height and slope measurements of

  17. Explosive mafic volcanism on Earth and Mars

    NASA Technical Reports Server (NTRS)

    Gregg, Tracy K. P.; Williams, Stanley N.

    1993-01-01

    Deposits within Amazonia Planitia, Mars, have been interpreted as ignimbrite plains on the basis of their erosional characteristics. The western flank of Hecates Tholus appears to be mantled by an airfall deposit, which was produced through magma-water interactions or exsolution of magmatic volatiles. Morphologic studies, along with numerical and analytical modeling of Martian plinian columns and pyroclastic flows, suggest that shield materials of Tyrrhena and Hadriaca paterae are composed of welded pyroclastic flows. Terrestrial pyroclastic flows, ignimbrites, and airfall deposits are typically associated with silicic volcanism. Because it is unlikely that large volumes of silicic lavas have been produced on Mars, we seek terrestrial analogs of explosives, mafic volcanism. Plinian basaltic airfall deposits have been well-documented at Masaya, Nicaragua, and basaltic ignimbrite and surge deposits also have been recognized there. Ambrym and Yasour, both in Vanuatu, are mafic stratovolcanioes with large central calderas, and are composed of interbedded basaltic pyrocalstic deposits and lava flows. Zavaritzki, a mafic stratovolcano in the Kurile Islands, may have also produced pyroclastic deposits, although the exact nature of these deposits in unknown. Masaya, Ambrym and Yasour are known to be located above tensional zones. Hadriaca and Tyrrhena Paterae may also be located above zones of tension, resulting from the formation and evolution of Hellas basin, and, thus, may be directly analogous to these terrestrial mafic, explosive volcanoes.

  18. Channels and valley networks. [of planet Mars surface

    NASA Technical Reports Server (NTRS)

    Baker, Victor R.; Carr, Michael H.; Gulick, Virginia C.; Williams, Cameron R.; Marley, Mark S.

    1992-01-01

    Attention is given to Martian channels and valley networks, since they have become a principal element of evidence to the effect that the Martian atmosphere evolved from an early volatile-rich state to its present condition. The outflow channels are relatively young, later Hesperian or Amazonian in age. They formed by immense outbursts of fluid from subsurface sources. Complexity in outflow-channel morphology was generated by varying amounts of sediment and ice in the aqueous-fluid flow systems. The overall cataclysmic-flood morphology may thus be locally transitional to morphologies generated by ice and debris flowage. Although local areas of valley networks, such as on Alba Patera, formed coevally with outflow channel activity, regionally extensive networks dominate in the heavily cratered terrains. The morphology of many valleys suggests genesis by ground-water sapping; for some valleys, surface runoff may have been more important.

  19. Mars gravity - Additional resolution from Viking Orbiter I

    NASA Technical Reports Server (NTRS)

    Sjogren, W. L.; Wimberly, R. N.; Cain, D. L.; Brenkle, J. P.

    1978-01-01

    Doppler radio tracking data taken from Viking Orbiter I at a 300 km periapsis altitude are now capable of resolving shorter wavelength features such as Olympus Mons and Alba Patera. The number of data is limited as is the area of high resolution which forms a narrow band near 35 deg N latitude. The masses of 71 disks, placed in a geometric pattern on the surface, were estimated. Location of each disk, the mass estimate, and the corresponding uncertainty are given for each disk mass included in the estimator. The new gravity results are compared with previous gravity reductions. The corresponding acceleration surface at 350 km altitude is displayed. It is concluded that systematic postfit residuals imply that further information can be extracted with more detailed modeling.

  20. Volcanic history, geologic analysis and map of the Prometheus Patera region on Io

    USGS Publications Warehouse

    Leone, G.; Gerard, Davies A.; Wilson, L.; Williams, D.A.; Keszthelyi, L.P.; Jaeger, W.L.; Turtle, E.P.

    2009-01-01

    Data from Jupiter's moon Io returned by the Galileo spacecraft have been used to create a geologic map of Prometheus Patera, its associated flow field, and nearby features. We have identified the location of the vent that fed the Prometheus flow field during the Galileo epoch in the north-eastern portion of the main Prometheus flow field. This vent is the probable source of a small sulphur-rich plume. Previous studies suggested that the vent may be atop a tectonic fault but we find that the vent is offset from the putative fault. It is plausible that, in the past, magma exploited the fault to reach the surface at Prometheus Patera, but subsequent magma cooling in the conduit could have caused an obstruction preventing further eruptions from providing significant contributions to the Prometheus flow field. We also speculate on how a new Prometheus plumbing system may be fed by mafic magmas after melt stalls in magma reservoirs during its ascent through the lithosphere from the mantle. ?? 2009 Elsevier B.V.

  1. Volcanic history, geologic analysis and map of the Prometheus Patera region on Io

    USGS Publications Warehouse

    Leone, Giovanni; Davies, Ashley G.; Wilson, Lionel; Williams, David A.; Keszthelyi, Laszlo P.; Jaeger, Windy L.; Turtle, Elizabeth P.

    2009-01-01

    Data from Jupiter's moon Io returned by the Galileo spacecraft have been used to create a geologic map of Prometheus Patera, its associated flow field, and nearby features. We have identified the location of the vent that fed the Prometheus flow field during the Galileo epoch in the north-eastern portion of the main Prometheus flow field. This vent is the probable source of a small sulphur-rich plume. Previous studies suggested that the vent may be atop a tectonic fault but we find that the vent is offset from the putative fault. It is plausible that, in the past, magma exploited the fault to reach the surface at Prometheus Patera, but subsequent magma cooling in the conduit could have caused an obstruction preventing further eruptions from providing significant contributions to the Prometheus flow field. We also speculate on how a new Prometheus plumbing system may be fed by mafic magmas after melt stalls in magma reservoirs during its ascent through the lithosphere from the mantle.

  2. Io: Charting thermal emission variability with the Galileo NIMS Io Thermal Emission Database (NITED): Loki Patera

    NASA Astrophysics Data System (ADS)

    Davies, A. G.; Veeder, G. J.; Matson, D. L.; Johnson, T. V.

    2012-01-01

    We have calculated the ≈5-μm radiant flux for every volcanic hot spot in every one of the 190 Galileo Near-Infrared Mapping Spectrometer (NIMS) tube observations of Io obtained between 28 June 1996 and 16 October 2001 in order to determine the variability of thermal emission from Io's volcanoes at local, regional and global scales, and to identify individual eruption episodes where thermal emission waxes and wanes. The resulting NIMS Io Thermal Emission Database (NITED) allows the comparison of activity at individual volcanoes and different regions of Io. The database contains over 1000 measurements of radiant flux at approximately 5 μm, corrected for emission angle, range to target and incident sunlight (where necessary). We examine the data for Loki Patera, Io's most powerful volcano. For data acquired in local darkness we use two-temperature fits to nighttime spectra and prior knowledge of emitting area to determine total radiated thermal emission. For other data we use the constancy of the integrated thermal emission spectrum to determine total thermal emission from measurements of radiant flux at 5 μm. As seen by NIMS, total thermal emission from Loki Patera varies between 7600 GW and 17000 GW. We revise upwards previous estimates of thermal emission from NIMS data. NIMS 3.5-μm radiant fluxes (both measured and estimated) are consistent with measurements from ground-based telescopes. This work highlights the value of NITED as a research tool.

  3. MC-3 Arcadia Region

    NASA Technical Reports Server (NTRS)

    1994-01-01

    Mars digital-image mosaic merged with color of the MC-3 quadrangle, Arcadia region of Mars. The southern part contains the large shield volcano, Alba Patera, and the highly faulted Tempe Terra province, which includes many small volcanoes. The northern part is dominated by relatively smooth plains. Latitude range 30 to 65 degrees, longitude range 60 to 120 degrees.

  4. Earth-like sand fluxes on Mars.

    PubMed

    Bridges, N T; Ayoub, F; Avouac, J-P; Leprince, S; Lucas, A; Mattson, S

    2012-05-09

    Strong and sustained winds on Mars have been considered rare, on the basis of surface meteorology measurements and global circulation models, raising the question of whether the abundant dunes and evidence for wind erosion seen on the planet are a current process. Recent studies showed sand activity, but could not determine whether entire dunes were moving--implying large sand fluxes--or whether more localized and surficial changes had occurred. Here we present measurements of the migration rate of sand ripples and dune lee fronts at the Nili Patera dune field. We show that the dunes are near steady state, with their entire volumes composed of mobile sand. The dunes have unexpectedly high sand fluxes, similar, for example, to those in Victoria Valley, Antarctica, implying that rates of landscape modification on Mars and Earth are similar.

  5. Relationships Between Paterae, Mountains, and Hotspots on Io from a Global Database

    NASA Technical Reports Server (NTRS)

    Radebaugh, J.; Jaeger, W. L.; Keszthelyi, L. P.; Turtle, E. P.; Milazzo, M. P.; Perry, J.; McEwen, A. S.; Lopes, R.; Davies, A. G.; Geissler, P.

    2004-01-01

    Now that the Galileo spacecraft s tour of the Jupiter system is over, we seek to integrate all available datasets in the hopes of understanding Io as completely as possible. We have compiled information about the morphologies and locations of paterae (volcano-tectonic depressions), mountains, and hotspots on Io in a single database. It is our hope that an analysis of the spatial and temporal relationships between these features will provide more indications of the nature of the crust of Io and the mechanisms leading to these features formation. Since Io s tidal heat escapes through its crust, more knowledge about the crust will lead to an understanding of internal processes, such as magma generation and delivery to the surface, and magnitude and orientation of internal stresses.

  6. Effusion Rate Variability at Zamama, Culann, Tupan Patera and Prometheus on Io during the Galileo Era

    NASA Astrophysics Data System (ADS)

    Davies, A. G.; Ennis, M. E.

    2011-10-01

    Zamama, Culann, and Tupan Patera are three large, persistent volcanic centers on the jovian moon Io. As part of an ongoing project to quantify contributions from individual volcanic centers to Io's thermal budget, we have quantified the radiant flux and effusion rates from all suitable observations made by the Galileo Near Infrared Mapping Spectrometer (NIMS) of these volcanoes [1], in some cases filling omissions in previous analyses. Eruption rates at these three volcanoes are on the order of 30 m3 s-1, consistent with a previous analysis of NIMS observations of Prometheus [2], and nearly an order of magnitude greater than Kilauea volcano, Hawai'i, Earth's most active volcano. We propose that future missions to the jovian system could better constrain activity at these volcanoes and others where similar styles of activity are taking place by obtaining data on a time scale of, ideally, at least one observation per day.

  7. Gish Bar Patera, Io: Geology and Volcanic Activity, 1996-2001

    NASA Technical Reports Server (NTRS)

    Perry, Jason; Radebaugh, Jani; Lopes, Rosaly; McEwen, Alfred; Keszthelyi, Laszlo

    2003-01-01

    Since the two Voyagers passed by Jupiter in 1979, it has been known that volcanic activity is ubiquitous on the surface of Io. With over 400 volcanic centers, Io is even more volcanically active than the earth with massive flood basalt-style eruptions and komatitite lavas a common occurrence. Additionally, some volcanoes appear to be giant lava lakes, with violent activity churning the crust of the lake for periods of 20 years or more. Finally, sulfur is believed to play a large role in Io's volcanism, be it as a primary lava or as a secondary product of large, high-temperature eruptions. By studying one volcano in particular, Gish Bar Patera, one can observe many of these characteristics in one volcanic center.

  8. Chronology, Eruption Duration, and Atmospheric Contribution of the Martian Volcano Apollinaris Patera

    USGS Publications Warehouse

    Robinson, M.S.; Mouginis-Mark, P. J.; Zimbelman, J.R.; Wu, S.S.C.; Ablin, K.K.; Howington-Kraus, A. E.

    1993-01-01

    Geologic mapping, thermal inertia measurements, and an analysis of the color (visual wavelengths) of the martian volcano Apollinaris Patera indicate the existence of two different surface materials, comprising an early, easily eroded edifice, and a more recent, competent fan on the southern flank. A chronology of six major events that is consistent with the present morphology of the volcano has been identified. We propose that large scale explosive activity occurred during the formation of the main edifice and that the distinctive fan on the southern flank appears to have been formed by lavas of low eruptive rate similar to those that form compound pahoehoe flow fields on Earth. A basal escarpment typically 500 m in relief and morphologically similar to the one surrounding Olympus Mons was produced between the formation of the main edifice and the fan, indicating multistage eruptions over a protracted period of time. Contact relations between the volcanic units and the adjacent chaotic material indicate that formation of the chaotic material occurred over an extended period of time and may be related to the volcanic activity that formed Apollinaris Patera. Stereophotogrammetric measurements permit the volume of the volcano to be estimated at 105 km3. From this volume measurement and an inferred eruption rate (1.5 ?? 10-2 km3 yr-1) we estimate the total eruption duration for the main edifice to be ???107 yrs. Plausible estimates of the exsolved volatile content of the parent magma imply that greater than 1015 kg of water vapor was released into the atmosphere as a consequence of this activity. This large amount of water vapor as well as other exsolved gases must have had a significant impact on local, and possibly global, climatic conditions. ?? 1993 Academic Press. All rights reserved.

  9. Highly oxygenated sesquiterpenes in Artemisia alba Turra.

    PubMed

    Todorova, Milka; Trendafilova, Antoaneta; Danova, Kalina; Simmons, Luke; Wolfram, Evelyn; Meier, Beat; Riedl, Rainer; Evstatieva, Luba

    2015-02-01

    Ten new sesquiterpene alcohols of which seven germacranes, a eudesmane, a guaiane and an oplopane were isolated from the aerial parts of Artemisia alba Turra. Their structures and relative stereochemistry were elucidated by spectral methods ((1)H and (13)C NMR, COSY, HSQC, HMBC, NOESY, and MS). In addition, the known 7-hydroxycadin-4-en-3-one, centaureidin and axillarin were found for the first time in the studied species.

  10. Supervolcanoes Within an Ancient Volcanic Province in Arabia Terra, Mars

    NASA Technical Reports Server (NTRS)

    Michalski, Joseph. R.; Bleacher, Jacob E.

    2014-01-01

    Several irregularly shaped craters located within Arabia Terra, Mars represent a new type of highland volcanic construct and together constitute a previously unrecognized martian igneous province. Similar to terrestrial supervolcanoes, these low-relief paterae display a range of geomorphic features related to structural collapse, effusive volcanism, and explosive eruptions. Extruded lavas contributed to the formation of enigmatic highland ridged plains in Arabia Terra. Outgassed sulfur and erupted fine-grained pyroclastics from these calderas likely fed the formation of altered, layered sedimentary rocks and fretted terrain found throughout the equatorial region. Discovery of a new type of volcanic construct in the Arabia volcanic province fundamentally changes the picture of ancient volcanism and climate evolution on Mars. Other eroded topographic basins in the ancient Martian highlands that have been dismissed as degraded impact craters should be reconsidered as possible volcanic constructs formed in an early phase of widespread, disseminated magmatism on Mars.

  11. Supervolcanoes within an ancient volcanic province in Arabia Terra, Mars.

    PubMed

    Michalski, Joseph R; Bleacher, Jacob E

    2013-10-03

    Several irregularly shaped craters located within Arabia Terra, Mars, represent a new type of highland volcanic construct and together constitute a previously unrecognized Martian igneous province. Similar to terrestrial supervolcanoes, these low-relief paterae possess a range of geomorphic features related to structural collapse, effusive volcanism and explosive eruptions. Extruded lavas contributed to the formation of enigmatic highland ridged plains in Arabia Terra. Outgassed sulphur and erupted fine-grained pyroclastics from these calderas probably fed the formation of altered, layered sedimentary rocks and fretted terrain found throughout the equatorial region. The discovery of a new type of volcanic construct in the Arabia volcanic province fundamentally changes the picture of ancient volcanism and climate evolution on Mars. Other eroded topographic basins in the ancient Martian highlands that have been dismissed as degraded impact craters should be reconsidered as possible volcanic constructs formed in an early phase of widespread, disseminated magmatism on Mars.

  12. Spatially Resolved M-band Emission from Io's Loki Patera-Fizeau Imaging at the 22.8 m LBT

    NASA Astrophysics Data System (ADS)

    Conrad, Albert; de Kleer, Katherine; Leisenring, Jarron; La Camera, Andrea; Arcidiacono, Carmelo; Bertero, Mario; Boccacci, Patrizia; Defrère, Denis; de Pater, Imke; Hinz, Philip; Hofmann, Karl-Heinz; Kürster, Martin; Rathbun, Julie; Schertl, Dieter; Skemer, Andy; Skrutskie, Michael; Spencer, John; Veillet, Christian; Weigelt, Gerd; Woodward, Charles E.

    2015-05-01

    The Large Binocular Telescope Interferometer mid-infrared camera, LMIRcam, imaged Io on the night of 2013 December 24 UT and detected strong M-band (4.8 μm) thermal emission arising from Loki Patera. The 22.8 m baseline of the Large Binocular Telescope provides an angular resolution of ˜32 mas (˜100 km at Io) resolving the Loki Patera emission into two distinct maxima originating from different regions within Loki’s horseshoe lava lake. This observation is consistent with the presence of a high-temperature source observed in previous studies combined with an independent peak arising from cooling crust from recent resurfacing. The deconvolved images also reveal 15 other emission sites on the visible hemisphere of Io including two previously unidentified hot spots.

  13. Classification of volcanoes of the Kane Patera Quadrangle of Io: Proportions of lava flows and pyroclastic flows

    NASA Technical Reports Server (NTRS)

    Elston, W. E.

    1984-01-01

    Voyager 1 images show 14 volcanic centers wholly or partly within the Kane Patera quadrangle of Io, which are divided into four major classes: (1) shield with parallel flows; (2) shield with early radial fan shapd flows; (3) shield with radial fan shaped flows, surfaces of flows textured with longitudinal ridges; and (4) depression surrounded by plateau-forming scarp-bounded, untextured deposits. The interpretation attempted here hinges largely on the ability to distinguish lava flows from pyroclastic flows by remote sensing.

  14. The Alba ray tracing code: ART

    NASA Astrophysics Data System (ADS)

    Nicolas, Josep; Barla, Alessandro; Juanhuix, Jordi

    2013-09-01

    The Alba ray tracing code (ART) is a suite of Matlab functions and tools for the ray tracing simulation of x-ray beamlines. The code is structured in different layers, which allow its usage as part of optimization routines as well as an easy control from a graphical user interface. Additional tools for slope error handling and for grating efficiency calculations are also included. Generic characteristics of ART include the accumulation of rays to improve statistics without memory limitations, and still providing normalized values of flux and resolution in physically meaningful units.

  15. Temperature, age and crust thickness distributions of Loki Patera on Io: implications for resurfacing mechanism

    NASA Technical Reports Server (NTRS)

    Davies, A. G.

    2003-01-01

    A high-spatial-resolution, multi-wavelength observation by the Galileo NIMS instrument has been analysed to determine the temperature and area distribution of a large portion of the ionian volcano Loki Patera. The temperatures of the cooler components from a two-temperature fit to the data can be used to determine ages of the surface. The age of the floor along a profile across the floor of the caldera ranges from 10 to 80 days. This puts the start of the resurfacing in July/early August 2001, yielding a resurfacing rate of approximately 1 km/day, with the new lava spreading from the SW corner of the caldera in a NE direction. This rate is consistent with resurfacing by foundering of the crust on a lava lake. However,the temperature distribution may also result from the emplacement of flows. Implied crust thicknesses (derived using a lava cooling model) range from 2.6 to 0.9 m.

  16. Tidal Dissipation in Basalt Magma Chambers - Implications for Io's Loki Patera and Icy Satellite Cores

    NASA Astrophysics Data System (ADS)

    Castillo, J. C.; Matson, D. L.; Davies, A. G.; Johnson, T. V.; Veeder, G. J.

    2006-05-01

    We discuss tidal dissipation in molten basaltic magma and the results from model application to Io and Enceladus. Magma is a non-newtonian liquid with a complex rheology dependent on interactions between different phases: liquid, crystals and bubbles, resulting in a slurry with each component responding differently to temperature and stress. This study is based on results obtained for terrestrial basalts. For example, the evolution of crystal content as a function of temperature has been described for basalts [e.g., 1]. The behavior of cyclically stressed basalt has been observed in laboratory for frequencies corresponding to seismic waves between 1 and 200 sec. [e.g., 2-5]. While this frequency range is outside the range of dynamical frequencies considered in planetary sciences, these results show variations of the response as a function of the wavelength of the structure involved in the response. From the trend observed at low frequencies we extrapolate these data to tidal frequencies encountered at Io and Enceladus. We apply this result to a silicate magma chamber deep in Enceladus's core. Such a magma body has been proposed by Matson et al. [6, 7] as a heat source for keeping Enceladus warm over geological time and ultimately powering the observed volcanism [8]. We also apply the model to the 'magma sea' at Loki Patera [9] the source of 10-20% of Io's heat flow. In both cases we evaluate how much tidal dissipation can be produced. Our objectives are to chart the development and long-term evolution of magma chambers on bodies heavily influenced by tidal dissipation. From consideration of the relevant processes taking place over appropriate timescales, results show that self- regulation mechanisms are in place, such that crystal content and heat production remain in equilibrium over geological time. Our preliminary results support long-term preservation of a magma chamber in Enceladus' core. Coupled thermal-orbital modeling also indicates consistency between this

  17. Observations and temperatures of Io's Pele Patera from Cassini and Galileo spacecraft images

    USGS Publications Warehouse

    Radebaugh, J.; McEwen, A.S.; Milazzo, M.P.; Keszthelyi, L.P.; Davies, A.G.; Turtle, E.P.; Dawson, D.D.

    2004-01-01

    Pele has been the most intense high-temperature hotspot on Io to be continuously active during the Galileo monitoring from 1996-2001. A suite of characteristics suggests that Pele is an active lava lake inside a volcanic depression. In 2000-2001, Pele was observed by two spacecraft, Cassini and Galileo. The Cassini observations revealed that Pele is variable in activity over timescales of minutes, typical of active lava lakes in Hawaii and Ethiopia. These observations also revealed that the short-wavelength thermal emission from Pele decreases with rotation of Io by a factor significantly greater than the cosine of the emission angle, and that the color temperature becomes more variable and hotter at high emission angles. This behavior suggests that a significant portion of the visible thermal emission from Pele comes from lava fountains within a topographically confined lava body. High spatial resolution, nightside images from a Galileo flyby in October 2001 revealed a large, relatively cool (< 800 K) region, ringed by bright hotspots, and a central region of high thermal emission, which is hypothesized to be due to fountaining and convection in the lava lake. Images taken through different filters revealed color temperatures of 1500 ?? 80 K from Cassini ISS data and 1605 ?? 220 and 1420 ?? 100 K from small portions of Galileo SSI data. Such temperatures are near the upper limit for basaltic compositions. Given the limitations of deriving lava eruption temperature in the absence of in situ measurement, it is possible that Pele has lavas with ultramafic compositions. The long-lived, vigorous activity of what is most likely an actively overturning lava lake in Pele Patera indicates that there is a strong connection to a large, stable magma source region. ?? 2003 Elsevier Inc. All rights reserved.

  18. In vitro regeneration of Basella alba L

    NASA Technical Reports Server (NTRS)

    Edney, Norris Allen; Rizvi, Muhammad A.; Rizvi, Narjis F.

    1989-01-01

    Basella alba L. is a tropical vine used as a vegetable in some Asian and African countries. It has potential as a nontraditional crop for small family farms. A short day plant, it blooms during the fall, provided the temperatures are mild. In the southeastern U.S., the short days of fall are associated with subfreezing temperatures, and plants are killed before blooming. Attempts were made to regenerate the plant using tissue culture techniques. Several trials were conducted with different media, hormones, and explants. It was found that nodal segments on Gamborg medium regenerated shoots. Interaction studies of auxins and cytokinins indicated that its endogeneous auxin content might be high because callus proliferated in almost all treatments and roots initiated even when the medium was not supplemented with an auxin.

  19. Antioxidant Effect of Lippia alba (Miller) N. E. Brown

    PubMed Central

    Chies, Claire E.; Branco, Cátia S.; Scola, Gustavo; Agostini, Fabiana; Gower, Adriana E.; Salvador, Mirian

    2013-01-01

    Lippia alba is a shrub found in all regions of Brazil and other countries in South and Central America. L. alba exhibits variability among its different accessions, showing differences in morphology and in the composition of its essential oil. This study evaluated the phenolic profiles and the antioxidant activities of seven different accessions of L. alba. The seven accessions of L. alba studied exhibited an important phenolic content, and all accessions demonstrated antioxidant activity with different efficacies. The main flavonoids in all accessions were apigenin, luteolin, naringin and rutin. The Santa Vitória do Palmar accession exhibited higher naringin and total phenolic content. This extract was able to reduce hydrogen peroxide-induced oxidative damage in tissue homogenates of cerebellum, cerebral cortex, hippocampus and liver of Wistar rats. PMID:26784458

  20. Antioxidant Effect of Lippia alba (Miller) N. E. Brown.

    PubMed

    Chies, Claire E; Branco, Cátia S; Scola, Gustavo; Agostini, Fabiana; Gower, Adriana E; Salvador, Mirian

    2013-09-26

    Lippia alba is a shrub found in all regions of Brazil and other countries in South and Central America. L. alba exhibits variability among its different accessions, showing differences in morphology and in the composition of its essential oil. This study evaluated the phenolic profiles and the antioxidant activities of seven different accessions of L. alba. The seven accessions of L. alba studied exhibited an important phenolic content, and all accessions demonstrated antioxidant activity with different efficacies. The main flavonoids in all accessions were apigenin, luteolin, naringin and rutin. The Santa Vitória do Palmar accession exhibited higher naringin and total phenolic content. This extract was able to reduce hydrogen peroxide-induced oxidative damage in tissue homogenates of cerebellum, cerebral cortex, hippocampus and liver of Wistar rats.

  1. Antihepatotoxic activity of eclipta alba, tephrosia purpurea and boerhaavia diffusa.

    PubMed

    Murthy, V N; Reddy, B P; Venkateshwarlu, V; Kokate, C K

    1992-01-01

    Alcoholic and chloroform extracts of E. albaT. purpurea and B. diffusa were screened for antihepatotoxic activity. The extracts were given after the liver was damaged with CCl4. Liver function was assessed based on liver to boy weight ratio, pentobarbitone sleep time, serum levels of transaminase (SGPT, SGOT), alkaline phosphatase (SALP) and bilirubin. Alcoholic extract of E. alba was found to have good antihepatotoxic activity.

  2. [Quality assessment of sulfur-fumigated paeoniae alba radix].

    PubMed

    Wang, Zhao; Chen, Yu-Wu; Wang, Qiong; Sun, Lei; Xu, Wei-Yi; Jin, Hong-Yu; Ma, Shuang-Cheng

    2014-08-01

    The samples of sulfur-fumigated Paeoniae Alba Radix acquired both by random spot check from domestic market and self-production by the research group in the laboratory were used to evaluate the effects of sulphur fumigation on the quality of Paeoniae Alba Radix by comparing sulfur-fumigated degree and character, the content of paeoniflorin and paeoniflorin sulfurous acid ester, and changes of the fingerprint. We used methods in Chinese Pharmacopeia to evaluate the character of sulfur-fumigated Paeoniae Alba Radix and determinate the content of aulfur-fumigated paeoniflorin. LC-MS method was used to analyze paeoniflorin-converted products. HPLC fingerprint methods were established to evaluate the differences on quality by similarity. Results showed that fumigated Paeoniae Alba Radix became white and its unique fragrance disappeared, along with the production of pungent sour gas. It also had a significant effect on paeoniflorin content. As sulfur smoked degree aggravated, paeoniflorin content decreased subsequently, some of which turned into paeoniflorin sulfurous acid ester, and this change was not reversible. Fingerprint also showed obvious changes. Obviously, sulfur fumigation had severe influence on the quality of Paeoniae Alba Radix, but we can control the quality of the Paeoniae Alba Radix by testing the paeoniflorin sulfurous acid ester content.

  3. The Summer 1997 Eruption at Pillan Patera on Io: Implications for Ultrabasic Lava Flow Emplacement

    NASA Technical Reports Server (NTRS)

    Williams, David A.; Davies, Ashley G.; Keszthelyi, Laszlo P.; Greeley, Ronald

    2001-01-01

    Galileo data and numerical modeling were used to investigate the summer 1977 eruption at Pillan Patera on Io. This event, now defined as "Pillanian" eruption style, included a high-temperature (greater than 1600 C), possible ultrabasic , 140-km-high plume eruption that deposited dark, orthopyroxene-rich pyroclastic material over greater than 125,000 sq km, followed by emplacement of dark flow-like material over greater than 3100 sq km to the north of the caldera. We estimate that the high-temperature, energetic episode of this eruption had a duration of 52 - 167 days between May and September 1997, with peak eruption temperatures around June 28, 1997. Galileo 20 m/pixel images of part of the Pillan flow field show a wide-spread, rough, pitted surface that is unlike any flow surface we have seen before. We suggest that this surface may have resulted from: 1. A fractured lava crust formed during rapid, low-viscosity lava surging, perhaps including turbulent flow emplacement. 2. Disruption of the lava flow by explosive interaction with a volatile-rich substrate. or 3. A combination of 1 and 2 with or without accumulation of pyroclastic material on the surface. Well-developed flow lobes are observed, suggesting that this is a relatively distant part of the flow field.Shadow measurements at flow margins indicate a thickness of-8 - 10 m. We have modeled the emplacement of putative ultrabasic flow from the summer 1997 Pillan eruption using constraints from new Galileo data. Results suggest that either laminar sheet flows or turbulent channelized flows could have traveled 50 - 150 km on a flat, unobstructed surface, which is consistent with the estimated length of the Pillan flow field (approx. 60 km). Our modeling suggests low thermal erosion rates (less than 4.1 m/d), and that the formation of deep (greater than 20 m) erosion channels was unlikely, especially distal to the source. We calculate a volumetric flow rate of approx. 2 - 7 x 10(exp 3)cu m/s, which is greater

  4. Paenibacillus alba nov., isolated from peat soil.

    PubMed

    Kim, Hyun-Sook; Srinivasan, Sathiyaraj; Lee, Sang-Seob

    2015-06-01

    A white-colored bacterial strain designated J20-6(T) was isolated from peat soil collected in Russia. Based on the 16S rRNA gene sequence similarities, the strain J20-6(T) belonged to the genus Paenibacillus, and the closest relatives were Paenibacillus frigoriresistens YIM 016(T) (98.2 %), Paenibacillus alginolyticus DSM 5050T(T) (97.9 %), Paenibacillus chondroitinus DSM 5051(T) (97.4 %), Paenibacillus pocheonensis Gsoil 1138(T) (96.9 %), and Paenibacillus pectinilyticus RCB-08(T) (96.6 %). Cells are gram-positive, motile, facultative aerobic, endospore forming, and rod shaped. The cell wall contains MK-7 as the predominant menaquinone and meso-diaminopimelic acid as the diagnostic diamino acid. The major fatty acid is anteiso-C15:0, and the major polar lipids are diphosphatidylglycerol and phosphatidyl-ethanolamine. The DNA G+C content of the strain J20-6(T) was 49.9 mol %. The phenotypic, chemotaxonomic, and phylogenetic data clearly suggest that the strain J20-6(T) belongs to the novel member of the genus Paenibacillus, for which the name Paenibacillus alba sp. nov., is proposed. The type strain is J20-6(T) (=KEMC 7302-005(T) = JCM 18165(T)).

  5. Mars Landscapes

    NASA Video Gallery

    Spacecraft have studied the Martian surface for decades, giving Earthlings insights into the history, climate and geology of our nearest neighbor, Mars. These images are from "Mars Landscapes," a v...

  6. The Hindlimb Myology of Tyto alba (Tytonidae, Strigiformes, Aves).

    PubMed

    Mosto, M C

    2017-02-01

    This work is the first myological dissection performed in detail on the hindlimb of Tyto alba. Six specimens were dissected and their muscle masses were obtained. T. alba has the classical myological pattern present in other species of Strigiformes, such as a well-developed m. flexor digitorum longus and the absence of the m. plantaris, flexor cruris lateralis and ambiens. Also, T. alba lacks the m. extensor propius digiti III, m. extensor propius digiti IV and m. lumbricalis, present in the Strigidae. Hindlimb muscle mass accounts for 14.13% of total body mass, which is within the range of values of both nocturnal (Strigiformes) and diurnal (Falconidae and Accipitridae) raptors. This study provides important information for future studies related to functional morphology and ecomorphology.

  7. Spatial Distribution of Volcanic Hotspots and Paterae on Io: Implications for Tidal Heating Models and Magmatic Pathways

    NASA Technical Reports Server (NTRS)

    Hamilton, C. W.; Beggan, C. D.; Lopes, R.; Williams, D. A.; Radenbaugh, J.

    2011-01-01

    Io, the innermost of Jupiter's Galilean satellites, is the most volcanically active body in the Solar. System. Io's global mean heat flow is approximately 2 W/square m, which is approximately 20 times larger than on Earth. High surface temperatures concentrate within "hotspots" and, to date, 172 Ionian hotspots have been identified by spacecraft and Earth-based telescopes. The Laplace resonance between Io, Europa, and Ganymede maintains these satellites in noncircular orbits and causes displacement of their tidal bulges as the overhead position of Jupiter changes for each moon. Gravitational interactions between Jupiter and Io dominate the orbital evolution of the Laplacian system and generate enormous heat within to as tidal energy is dissipated. If this energy were transferred out of Io at the same rate as it is generated, then the associated surface heat flux would be 2.24 +/- 0.45 W/square m. This estimate is in good agreement with observed global heat flow, but to better constrain tidal dissipation mechanisms and infer how thermal energy is transferred to Io's surface, it is critical to closely examine the spatial distribution of volcanic features. End-member tidal dissipation models either consider that heating occurs completely in the mantle, or completely in the asthenosphere. Mixed models typically favor one-third mantle and two-thirds asthenosphere heating. Recent models also consider the effects of mantle-asthenosphere boundary permeability and asthenospheric instabilities. Deep-mantle heating models predict maximum surface heat flux near the poles, whereas asthenosphere heating models predict maxima near the equator-particularly in the Sub-Jovian and Anti-Jovian hemispheres, with smaller maxima occurring at orbit tangent longitudes. Previous studies have examined the global distribution of Ionian hotspots and patera (i.e., irregular or complex craters with scalloped edges that are generally interpreted to be volcanic calderas), but in this study, we

  8. Mars geologic mapping program: Review and highlights

    NASA Astrophysics Data System (ADS)

    Scott, David H.

    1991-06-01

    The Mars Geologic Mapping (MGM) Program was introduced by NASA in 1987 as a new initiative in the Planetary Geology and Geophysics (PGG) Program. The overall purpose of the program is to support research on topical science problems that address specific questions. Among the objectives of the project are: (1) to produce highly detailed geologic maps that will greatly increase the knowledge of the materials and processes that have contributed to the evolutionary history of Mars; (2) to define areas of special interest for possible future investigation by planned missions (Mars Observer, Mars Sample Return); and (3) to maintain the interest of the planetary community in the development of new concepts and the re-evaluation of Martian geology as new data in usable form become available. Some interesting highlights of the geologic mapping indicate that multiple flood episodes occurred at different times during the Hesperian Period in both Kasei and Maja Valles. Studies of small channels in the Memnonia, Mangala, and Tharsis regions show that fluvial events appear to have occurred during the Amazonian Period at equatorial latitudes. Flood waters occurred during the Amazonian Period at equatorial latitudes. Flood waters from Mangala Valles may have seeped into surficial materials with the subsequent development of numerous sapping channels and debris flows; this suggests that the ancient highland terrain consists of relatively unconsolidated materials. Multiple layers were observed for the first time in the ridged plains lava flows covering large areas of Lunae Planum; some wrinkle ridges in this area are associated with grabens and collapse volcanic units at Hadriaca and Tyrrhena Paterae indicates that the units may have been emplaced by gravity-driven pyroclastic flows. Unlike the north polar layered deposits, those in the south polar region show no angular unconformities or evidence of faulting and folding. Water ice in the south polar layered deposits may be protected

  9. Mars geologic mapping program: Review and highlights

    NASA Technical Reports Server (NTRS)

    Scott, David H.

    1991-01-01

    The Mars Geologic Mapping (MGM) Program was introduced by NASA in 1987 as a new initiative in the Planetary Geology and Geophysics (PGG) Program. The overall purpose of the program is to support research on topical science problems that address specific questions. Among the objectives of the project are: (1) to produce highly detailed geologic maps that will greatly increase the knowledge of the materials and processes that have contributed to the evolutionary history of Mars; (2) to define areas of special interest for possible future investigation by planned missions (Mars Observer, Mars Sample Return); and (3) to maintain the interest of the planetary community in the development of new concepts and the re-evaluation of Martian geology as new data in usable form become available. Some interesting highlights of the geologic mapping indicate that multiple flood episodes occurred at different times during the Hesperian Period in both Kasei and Maja Valles. Studies of small channels in the Memnonia, Mangala, and Tharsis regions show that fluvial events appear to have occurred during the Amazonian Period at equatorial latitudes. Flood waters occurred during the Amazonian Period at equatorial latitudes. Flood waters from Mangala Valles may have seeped into surficial materials with the subsequent development of numerous sapping channels and debris flows; this suggests that the ancient highland terrain consists of relatively unconsolidated materials. Multiple layers were observed for the first time in the ridged plains lava flows covering large areas of Lunae Planum; some wrinkle ridges in this area are associated with grabens and collapse volcanic units at Hadriaca and Tyrrhena Paterae indicates that the units may have been emplaced by gravity-driven pyroclastic flows. Unlike the north polar layered deposits, those in the south polar region show no angular unconformities or evidence of faulting and folding. Water ice in the south polar layered deposits may be protected

  10. Are sinuous ridges and channel networks in the equatorial Rahway Vallis region of Mars fluvioglacial in origin?

    NASA Astrophysics Data System (ADS)

    Ramsdale, J. D.; Balme, M. R.; Conway, S. J.; Gallagher, C.

    2013-09-01

    We have studied a network of channels and ridges that are key to understanding the extremely flat (sloping at 0.02° south-east) geomorphology of Rahway Vallis, south-west of Orcus Patera, Mars. The branching pattern of the ridge and channel system is consistent with a fluvial origin, with cross sections of the channel and banks being reminiscent of fluvial v-shaped valleys. Possible fluvial explanations for the sinuous ridges include inverted fluvial channels [e.g., 1] and eskers (sub-glacial, sediment-filled channels, e.g. [2]). Here, we present observations on the system and test the fluvial and fluvioglacial hypotheses.

  11. Identification and molecular characterization of an Alba-family protein from human malaria parasite Plasmodium falciparum

    PubMed Central

    Goyal, Manish; Alam, Athar; Iqbal, Mohd Shameel; Dey, Sumanta; Bindu, Samik; Pal, Chinmay; Banerjee, Anindyajit; Chakrabarti, Saikat; Bandyopadhyay, Uday

    2012-01-01

    We have investigated the DNA-binding nature as well as the function of a putative Alba (Acetylation lowers binding affinity) family protein (PfAlba3) from Plasmodium falciparum. PfAlba3 possesses DNA-binding property like Alba family proteins. PfAlba3 binds to DNA sequence non-specifically at the minor groove and acetylation lowers its DNA-binding affinity. The protein is ubiquitously expressed in all the erythrocytic stages of P. falciparum and it exists predominantly in the acetylated form. PfAlba3 inhibits transcription in vitro by binding to DNA. Plasmodium falciparum Sir2 (PfSir2A), a nuclear localized deacetylase interacts with PfAlba3 and deacetylates the lysine residue of N-terminal peptide of PfAlba3 specific for DNA binding. PfAlba3 is localized with PfSir2A in the periphery of the nucleus. Fluorescence in situ hybridization studies revealed the presence of PfAlba3 in the telomeric and subtelomeric regions. ChIP and ChIP ReChIP analyses further confirmed that PfAlba3 binds to the telomeric and subtelomeric regions as well as to var gene promoter. PMID:22006844

  12. Phytochemistry, pharmacology, and clinical trials of Morus alba.

    PubMed

    Chan, Eric Wei-Chiang; Lye, Phui-Yan; Wong, Siu-Kuin

    2016-01-01

    The present review is aimed at providing a comprehensive summary on the botany, utility, phytochemistry, pharmacology, and clinical trials of Morus alba (mulberry or sang shu). The mulberry foliage has remained the primary food for silkworms for centuries. Its leaves have also been used as animal feed for livestock and its fruits have been made into a variety of food products. With flavonoids as major constituents, mulberry leaves possess various biological activities, including antioxidant, antimicrobial, skin-whitening, cytotoxic, anti-diabetic, glucosidase inhibition, anti-hyperlipidemic, anti-atherosclerotic, anti-obesity, cardioprotective, and cognitive enhancement activities. Rich in anthocyanins and alkaloids, mulberry fruits have pharmacological properties, such as antioxidant, anti-diabetic, anti-atherosclerotic, anti-obesity, and hepatoprotective activities. The root bark of mulberry, containing flavonoids, alkaloids and stilbenoids, has antimicrobial, skin-whitening, cytotoxic, anti-inflammatory, and anti-hyperlipidemic properties. Other pharmacological properties of M. alba include anti-platelet, anxiolytic, anti-asthmatic, anthelmintic, antidepressant, cardioprotective, and immunomodulatory activities. Clinical trials on the efficiency of M. alba extracts in reducing blood glucose and cholesterol levels and enhancing cognitive ability have been conducted. The phytochemistry and pharmacology of the different parts of the mulberry tree confer its traditional and current uses as fodder, food, cosmetics, and medicine. Overall, M. alba is a multi-functional plant with promising medicinal properties.

  13. Onion and weed response to mustard (Sinapis alba) seed meal

    Technology Transfer Automated Retrieval System (TEKTRAN)

    Weed control in organic onion production is often difficult and expensive, requiring numerous cultivations and extensive hand-weeding. Onion safety and weed control with mustard seed meal (MSM) derived from Sinapis alba was evaluated in greenhouse and field trials. MSM applied at 110, 220, and 440 g...

  14. Chemical composition and antigenotoxic properties of Lippia alba essential oils

    PubMed Central

    López, Molkary Andrea; Stashenko, Elena E.; Fuentes, Jorge Luis

    2011-01-01

    The present work evaluated the chemical composition and the DNA protective effect of the essential oils (EOs) from Lippia alba against bleomycin-induced genotoxicity. EO constituents were determined by Gas Chromatography/Mass Spectrometric (GC-MS) analysis. The major compounds encountered being citral (33% geranial and 25% neral), geraniol (7%) and trans-β-caryophyllene (7%) for L. alba specimen COL512077, and carvone (38%), limonene (33%) and bicyclosesquiphellandrene (8%) for the other, COL512078. The genotoxicity and antigenotoxicity of EO and the compounds citral, carvone and limonene, were assayed using the SOS Chromotest in Escherichia coli. The EOs were not genotoxic in the SOS chromotest, but one of the major compound (limonene) showed genotoxicity at doses between 97 and 1549 mM. Both EOs protected bacterial cells against bleomycin-induced genotoxicity. Antigenotoxicity in the two L. alba chemotypes was related to the major compounds, citral and carvone, respectively. The results were discussed in relation to the chemopreventive potential of L. alba EOs and its major compounds. PMID:21931523

  15. Chemical composition and antigenotoxic properties of Lippia alba essential oils.

    PubMed

    López, Molkary Andrea; Stashenko, Elena E; Fuentes, Jorge Luis

    2011-07-01

    The present work evaluated the chemical composition and the DNA protective effect of the essential oils (EOs) from Lippia alba against bleomycin-induced genotoxicity. EO constituents were determined by Gas Chromatography/Mass Spectrometric (GC-MS) analysis. The major compounds encountered being citral (33% geranial and 25% neral), geraniol (7%) and trans-β-caryophyllene (7%) for L. alba specimen COL512077, and carvone (38%), limonene (33%) and bicyclosesquiphellandrene (8%) for the other, COL512078. The genotoxicity and antigenotoxicity of EO and the compounds citral, carvone and limonene, were assayed using the SOS Chromotest in Escherichia coli. The EOs were not genotoxic in the SOS chromotest, but one of the major compound (limonene) showed genotoxicity at doses between 97 and 1549 mM. Both EOs protected bacterial cells against bleomycin-induced genotoxicity. Antigenotoxicity in the two L. alba chemotypes was related to the major compounds, citral and carvone, respectively. The results were discussed in relation to the chemopreventive potential of L. alba EOs and its major compounds.

  16. Global near-IR maps from Gemini-N and Keck in 2010, with a special focus on Janus Patera and Kanehekili Fluctus

    NASA Astrophysics Data System (ADS)

    de Pater, Imke; Davies, Ashley Gerard; McGregor, Alistair; Trujillo, Chad; Ádámkovics, Máté; Veeder, Glenn J.; Matson, Dennis L.; Leone, Giovanni

    2014-11-01

    We have imaged Io in the near-infrared (1-5 μm) with adaptive optics on the 10-m W.M. Keck II and the Gemini North telescopes. We have constructed global maps from the data taken in 2010. Although numerous hot spots are visible, the maps are dominated by two volcanic centers: Loki Patera and Kanehekili Fluctus. We have examined in detail the thermal emission from Janus Patera and Kanehekili Fluctus using images obtained between 2003 and 2010, and have created a timeline of volcanic activity at these locations utilizing data from a wide variety of sources. Based on our data and this timeline we find that the thermal emission from Janus Patera is relatively steady, indicative of an active lava lake. The thermal emission from Kanehekili Fluctus, however, is quite variable, and is indicative of the emplacement of extensive lava flows. In 2010, the thermal emission from this location was ∼10 times higher than ever seen before, indicative of a particularly voluminous eruption of lava.

  17. Spatially resolved observations of the forbidden SO aΔ→XΣ rovibronic transition on Io during an eclipse and a volcanic eruption at Ra Patera

    NASA Astrophysics Data System (ADS)

    de Pater, Imke; Laver, Conor; Marchis, Franck; Roe, Henry G.; Macintosh, Bruce A.

    2007-11-01

    We report observations of Io that were conducted on UT 12 November 2002 with the NIRSPEC spectrometer, coupled to the adaptive optics system, on the 10-m Keck II telescope. We detected a bright eruption in the Ra Patera area, with a color (H-K' band) temperature of 1031±110 K over an effective area of 1.5±0.2 km. The eruption was associated with a hot plume, which revealed itself through SO emission at a rate of (9±3)×10 photonss, about 10-15% of Io's total SO flux at the time. The rotational temperature was 700±150 K. No significant SO emission was received from Io's northern hemisphere (north of Ra Patera/Loki); roughly 50% of the total SO emission came from the equatorial region (including Ra Patera, Janus and Loki), and ˜40% came from the south. The rotational temperatures typically measured between 600 and 1000 K. The emissions are most likely produced by SO molecules ejected out of volcanic vents in the excited aΔ state. Our narrow band images that span the SO emission band suggest that a source near Io's south pole, Nemea, may be a source of some of the southern SO emissions.

  18. Multihued Mars

    NASA Technical Reports Server (NTRS)

    2004-01-01

    This image taken at JPL shows the panoramic camera used onboard both Mars Exploration Rovers. The panel to the lower right highlights the multicolored filter wheel that allows the camera to see a rainbow of colors, in addition to infrared bands of light. By seeing Mars in all its colors, scientists can gain insight into the different minerals that constitute its rocks and soil.

  19. Development of a novel set of microsatellite markers for Lippia alba (Verbenaceae).

    PubMed

    Rocha, D S; Santos, C P; Bajay, M M; Campos, J B; Blank, A F; Pinheiro, J B; Zucchi, M I

    2015-02-03

    Microsatellite primers were developed and optimized for Lippia alba to characterize the L. alba germplasm bank of Universidade de São Paulo. A genomic library enabled the design of 9 microsatellite primers. Six of the 9 primers yielded polymorphic products, which defined 2 groups in the bank. The data provide support to characterize germplasm banks, genetic breeding programs for L. alba, and other genetic diversity studies and classifications of species in the genus Lippia.

  20. Rippled Mars

    NASA Technical Reports Server (NTRS)

    2004-01-01

    29 July 2004 Hundreds of large ripples or small dunes cover the landscape in the Terra Tyrrhena region of Mars in this Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image. The winds responsible for these dunes blew from the north-northwest (top/upper left). This scene is located near 8.8oS, 252.8oW, and covers an area about 3 km (1.9 mi) wide. Sunlight illuminates the terrain from the left.

  1. The analyst at work: two sessions with Alba.

    PubMed

    Bolognini, Stefano

    2002-08-01

    In this paper, the author presents clinical material that relates to two sessions with a patient called Alba. This analytic work, being of a somewhat unusual character, lends itself to discussion, the author feels, since the technical choices made are undoubtedly very personal and he believes many colleagues might have done things differently. The author endeavours to enrich the account of the sessions with his concomitant thoughts, so as to supply colleagues with the elements, atmosphere and developments of his internal workshop.

  2. LINEA ALBA COLLAGEN ASSESSMENT IN MORBIDLY OBESE PATIENTS

    PubMed Central

    GROSSI, João Vicente Machado; NICOLA, Felipe Fernandes; ZEPEDA, Ivan Alberto; BECKER, Martina; TRINDADE, Eduardo Neubarth; DIEMEN, Vinicius Von; CAVAZZOLA, Leandro Totti; TRINDADE, Manoel Roberto Maciel

    2016-01-01

    ABSTRACT Background: The evaluation of collagen in the abdominal wall has been increasingly studied because of the relevance on collagen in the healing process after laparotomy. Aim: To evaluate the amount of collagen in the linea alba of patients undergoing laparotomic bariatric surgery and comparing with non-obese cadavers. Methods: Were evaluated 88 samples of aponeurosis from abdominal linea alba of 44 obese patients (obesity group) and 44 non-obese cadavers (control group). The samples were collected in 2013 and 2104, and were sorted according to age (18-30, 31-45 and 46-60), gender, BMI, waist and cervical circumference, and subcutaneous tissue thickness. Material for biopsy was collected from the supraumbilical region of the linea alba for immunohistochemical analysis differentiating collagen type 1 and type 3 and the 1/3 ratio. Image-Pro Plus pixel counting software was used to measure the amount of collagen. Results: The obesity group evidenced mean age 44.11±9.90 years; 18-30 age group had three (6.8%) obese individuals; 31-45 had 22 (50%) and 46-60 had 19 (43.1%). Females were present in 81.8% (n=36); BMI (kg/m²) was 48.81±6.5; waist circumference (cm) was 136.761±13.55; subcutaneous tissue thickness (cm) 4.873±0.916. Considering age groups, gender and BMI, there were statistical differences in all tests when compared with the cadavers. Conclusion: The amount of collagen in the linea alba above the umbilical region in the morbidly obese patients was smaller than in the non-obese cadavers in the same age group. PMID:27683766

  3. Mars Underground News.

    NASA Astrophysics Data System (ADS)

    Edgett, K.

    Contents: Next entry to Mars (Mars Pathfinder and the microrover Sojourner). Hello, Mars, we're back! Mars Global Surveyor update. The Mars program - 2001 and beyond. Schedule of missions to Mars (as of June 11, 1997). Mars on the Web.

  4. Antiulcerogenic activity of Lippia alba (Mill.) N. E. Brown (Verbenaceae).

    PubMed

    Pascual, M E; Slowing, K; Carretero, M E; Villar, A

    2001-01-01

    Lippia alba (Mill.) N. E. Brown Verbenaceae, known popularly as 'Juanilama' or 'Salvia Sija', is prized widely in folk medicine in Guatemala. Its leaves are employed as an infusion and decoction as a remedy for stomach problems, dysentery, colds and cough, febrifuge, as well as a sedative and in spasmolitic remedies. The present study reports the effects of the infusion of L. alba on the rat gastric mucosa. The following behavioural parameters were evaluated: (a) gastric irritancy test in Wistar rats; (b) antiulcer activity, short term and long term; (c) acid secretion; (d) measurement of total proteins; (e) estimation of total protein bound and nonprotein sulfhydryl groups. Ranitidine (100 mg/kg, p.o.) was used as the reference antiulcer drug. Oral treatment with the infusion (12.5 g dry plant/kg) did not cause gastric irritancy in the rats treated during five consecutive days. In addition, the oral administration of L. alba was found to be effective at preventing gastric ulceration induced by indomethacin (50 mg/kg, p.o.) in rats in the short term (1 day) and long term (5 days).

  5. Mars Bowling

    NASA Video Gallery

    More than 140 fourth and fifth graders from Kraft Elementary School in Hampton learned how Newton's laws of motion apply to bowling and the Mars Curiosity rover during "The Science of Bowling," an ...

  6. Mars resources

    NASA Technical Reports Server (NTRS)

    Duke, Michael B.

    1986-01-01

    The most important resources of Mars for the early exploration phase will be oxygen and water, derived from the Martian atmosphere and regolith, which will be used for propellant and life support. Rocks and soils may be used in unprocessed form as shielding materials for habitats, or in minimally processed form to expand habitable living and work space. Resources necessary to conduct manufacturing and agricultural projects are potentially available, but will await advanced stages of Mars habitation before they are utilized.

  7. Exploring Mars

    NASA Astrophysics Data System (ADS)

    Breuil, Stéphanie

    2016-04-01

    Mars is our neighbour planet and has always fascinated humans as it has been seen as a potential abode for life. Knowledge about Mars is huge and was constructed step by step through numerous missions. It could be difficult to describe these missions, the associated technology, the results, the questions they raise, that's why an activity is proposed, that directly interests students. Their production is presented in the poster. Step 1: The main Mars feature and the first Mars explorations using telescope are presented to students. It should be really interesting to present "Mars Canals" from Percival Lowell as it should also warn students against flawed interpretation. Moreover, this study has raised the big question about extra-terrestrial life on Mars for the first time. Using Google Mars is then a good way to show the huge knowledge we have on the planet and to introduce modern missions. Step 2: Students have to choose and describe one of the Mars mission from ESA and NASA. They should work in pairs. Web sites from ESA and NASA are available and the teacher makes sure the main missions will be studied. Step 3: Students have to collect different pieces of information about the mission - When? Which technology? What were the main results? What type of questions does it raise? They prepare an oral presentation in the form they want (role play, academic presentation, using a poster, PowerPoint). They also have to produce playing cards about the mission that could be put on a timeline. Step 4: As a conclusion, the different cards concerning different missions are mixed. Groups of students receive cards and they have to put them on a timeline as fast as possible. It is also possible to play the game "timeline".

  8. Mars Pathfinder

    NASA Astrophysics Data System (ADS)

    Murdin, P.

    2000-11-01

    First of NASA's Discovery missions. Launched in December 1996 and arrived at Mars on 4 July 1997. Mainly intended as a technology demonstration mission. Used airbags to cushion the landing on Mars. The Carl Sagan Memorial station returned images of an ancient flood plain in Ares Vallis. The 10 kg Sojourner rover used an x-ray spectrometer to study the composition of rocks and travelled about 100 ...

  9. Whole-genome sequence of Nocardiopsis alba strain ATCC BAA-2165, associated with honeybees.

    PubMed

    Qiao, Jianjun; Chen, Lei; Li, Yongli; Wang, Jiangxin; Zhang, Weiwen; Chen, Shawn

    2012-11-01

    The actinomycete Nocardiopsis alba was reportedly associated with honeybees in separate occurrences. We report the complete genome of Nocardiopsis alba ATCC BAA-2165 isolated from honeybee guts. It will provide insights into the metabolism and genetic regulatory networks of this genus of bacteria that enable them to live in a range of environments.

  10. Parasiticidal effects of Morus alba root bark extracts against Ichthyophthirius multifiliis infecting grass carp

    Technology Transfer Automated Retrieval System (TEKTRAN)

    Ichthyophthirius multifiliis (Ich) is an important fish parasite that can result in significant losses in aquaculture. In order to find efficacious drugs to control Ich, the root bark of Morus alba, a traditional Chinese medicine, was evaluated for its antiprotozoal activity. The M. alba root bark w...

  11. Counter-Hegemonic Regionalism and Higher Education for All: Venezuela and the ALBA

    ERIC Educational Resources Information Center

    Muhr, Thomas

    2010-01-01

    This paper employs new regionalism theory and regulatory regionalism theory in its analysis and theorisation of the Bolivarian Alliance for the Peoples of Our America (ALBA) as a counter-hegemonic Latin American and Caribbean (LAC) regionalism. As (initially) the regionalisation of Venezuela's Bolivarian Revolution, ALBA is centred around the idea…

  12. Cracky Mars

    NASA Technical Reports Server (NTRS)

    2006-01-01

    21 September 2006 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows cracked, layered plains-forming material in the western part of Utopia Planitia, Mars. Investigators have speculated that ice might be -- or might once have been -- present in the ground, and changes in temperature and the amount of ice over time may have led to the formation of these cracks. But no one is certain just how these features formed.

    Location near: 45.0oN, 276.1oW Image width: 3 km (1.9 mi) Illumination from: lower left Season: Northern Spring

  13. Mars Topography

    NASA Technical Reports Server (NTRS)

    2001-01-01

    These maps are global false-color topographic views of Mars at different orientations from the Mars Orbiter Laser Altimeter (MOLA). The maps are orthographic projections that contain over 200,000,000 points and about 5,000,000 altimetric crossovers. The spatial resolution is about 15 kilometers at the equator and less at higher latitudes. The vertical accuracy is less than 5 meters. The right hand image view features the Hellas impact basin (in purple, with red annulus of high standing material). The left hand features the Tharsis topographic rise (in red and white). Note also the subtle textures associated with resurfacing of the northern hemisphere lowlands in the vicinity of the Utopia impact basin. These data were compiled by the Mars Orbiter Laser Altimeter (MOLA) Team led by David Smith at the Goddard Space Flight Center in Greenbelt, MD.

  14. Soil plant interactions of Populus alba in contrasting environments.

    PubMed

    Ciadamidaro, Lisa; Madejón, Engracia; Robinson, Brett; Madejón, Paula

    2014-01-01

    The effects of the Populus alba tree on different biochemical soil properties, growing in a contaminated area, were studied for two years under field conditions. Two types of trace element contaminated soils were studied: a neutral contaminated soil (NC) and an acid contaminated soil (AC). One neutral non-contaminated area was studied as control. Soil samples were collected at depths of 0-20 cm and 20-40 cm. Leaves and litter samples were analysed. The addition of organic matter, through root exudates and litter, contributed to an increase in soil pH, especially in acid soil. Microbial Biomass Carbon (MBC) was significantly increased by the presence of the trees in all studied areas, especially in the upper soil layer. Similar results were also observed for protease activity. Both MBC and Protease activity were more sensitive to contamination than β-glucosidase activity. These changes resulted in a decrease of available trace element concentrations in soil and in an improvement of soil quality after a 2-year study. The total concentration of Cd and Zn in soil did not increase over time due to litter deposition. Analysis of P. alba leaves did not show a significant nutritional imbalance and trace element concentrations were normal for plants, except for Cd and Zn. These results indicate that P. alba is suitable for the improvement of soil quality in riparian contaminated areas. However, due to the high Cd and Zn concentrations in leaves, further monitoring of this area is required.

  15. Installation, commissioning and performance of IDs installed at ALBA

    NASA Astrophysics Data System (ADS)

    Campmany, J.; Marcos, J.; Massana, V.; Becheri, F.; Gigante, J. V.; Colldelram, C.; Ribó, Ll

    2013-03-01

    The new synchrotron light source ALBA is currently starting regular operation. Up to 6 beamlines are using light produced by Insertion Devices. There are up to four types of IDs: 2 Apple-II undulators (EU62 and EU71) operating at low energies, one conventional wiggler (MPW80) operating in the range of 2 - 20 keV, two in-vacuum undulators (IVU21) operating in the range 5 - 30 keV and a superconducting wiggler (SCW30) operating in the range of (up to) 40 keV. The main IDs characteristics, their influence on the beam dynamics and a first characterization of their light will be presented.

  16. New triterpenoids from Morus alba L. stem bark.

    PubMed

    Ali, Abuzer; Ali, Mohd

    2013-01-01

    Two lupeol-type pentacyclic triterpenoids characterised as lup-20(29)-en-3β-ol-27-oic acid (moruslupenoic acid A) and lup-12, 20(29)-dien-3β-ol-26-oic acid (moruslupenoic acid B) and lanst-5, 24-dien-3β-yl acetate (moruslanosteryl acetate) along with the known triterpenoidal phytoconstituents α-amyrin acetate, β-amyrin-β-D-glucopyranoside and betulinic acid have been isolated from the stem bark of Morus alba L. (Moraceae). The structures of the isolated phytoconstituents were established on the basis of spectral data analysis and chemical means.

  17. The dynamics of pyroclastic density currents on Mars

    NASA Astrophysics Data System (ADS)

    Brand, B. D.; Clarke, A. B.

    2010-12-01

    The products of explosive volcanism have long been observed on the surface of Mars, and their corresponding dynamics, associated with phenomenon such as dike propagation, magma fragmentation, and eruption columns under Martian conditions, have been modeled with significant success (e.g., Wilson, L., J. W. Head (1994), Mars- Review and analysis of volcanic eruption theory and relationships to observed landforms, Rev. Geophy, 32, 221-263). However, the dynamics of pyroclastic density currents (PDCs) under Martian conditions is still poorly constrained. Our increasing capability to image the surface at high resolution, both from orbit and from rovers, presents an opportunity for more rigorous deposit observations and descriptions. For example, observations and measurements from Orbiters identify what have been interpreted as extensive aprons of volcanic ash deposits in several volcanic regions, namely those surrounding several southern highland patera, which have been interpreted as the deposits of PDCs. In addition the bedded deposits identified by the Spirit rover at “Home Plate,” an outcrop within the Columbia Hills in Gusev Crater, have been interpreted by many as the deposits of dilute pyroclastic density currents. This demonstrates that the need to understand the role of the Martian atmosphere on flow dynamics and depositional processes is much more important and relevant than it has been in the past. We have developed a quantitative, axi-symmetric model for flow of and sedimentation from a steady-state, vertically uniform dilute density current for application to PDCs on Earth and Mars (following Bursik, M. I., A. W. Woods, 1996, The dynamics and thermodynamics of large ash flows, Bull Volcan, 58, 175-193). The conservation of mass, momentum, and energy are solved simultaneously, and include the effects of atmospheric entrainment, particle sedimentation, basal friction, temperature changes, and variations in current thickness and density. For a given set of

  18. The variability of volcanic activity at Zamama, Culann, and Tupan Patera on Io as seen by the Galileo Near Infrared Mapping Spectrometer

    NASA Astrophysics Data System (ADS)

    Davies, Ashley Gerard; Ennis, Megan Elizabeth

    2011-09-01

    Zamama, Culann, and Tupan Patera are three large, persistent volcanic centers on the jovian moon Io. As part of an ongoing project to quantify contributions from individual volcanic centers to Io's thermal budget, we have quantified the radiant flux from all suitable observations made by the Galileo Near Infrared Mapping Spectrometer (NIMS) of these volcanoes, in some cases filling omissions in previous analyses. At Zamama, after a long period of cooling, we see a peak in thermal emission that corresponds with new plume activity. Subsequently, toward the end of the Galileo epoch, thermal emission from Zamama drops off in a manner consistent with a greatly reduced eruption rate and the cooling of emplaced flows. Culann exhibits possible episodic activity. We present the full Tupan Patera NIMS dataset and derive new estimates of thermal output and temporal behavior. Eruption rates at these three volcanoes are on the order of 30 m 3 s -1, consistent with a previous analysis of NIMS observations of Prometheus, and nearly an order of magnitude greater than Kilauea volcano, Hawai'i, Earth's most active volcano. We propose that future missions to the jovian system could better constrain activity at these volcanoes and others where similar styles of activity are taking place by obtaining data on a time scale of, ideally, at least one observation per day. Observations at similar or even shorter timescales are desirable during initial waxing phases of eruption episodes. These eruptions are identifiable from their characteristic spectral signatures and temporal behavior.

  19. Mars exploration.

    PubMed

    Carr, M H; Garvin, J

    2001-07-12

    An international flotilla of spacecraft are to be sent to Mars over the next decade in an effort to understand the planet's geology and climate history, and to determine whether some form of life ever started there. At least two spacecraft will be sent at each launch opportunity, and at times up to four spacecraft may be operating simultaneously at the planet.

  20. Mars 2003

    NASA Technical Reports Server (NTRS)

    2003-01-01

    MGS MOC Release No. MOC2-402, 25 June 2003

    The Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) experiment consists of 3 different cameras: a narrow angle imager that provides the black-and-white high resolution views (up to 1.4 meters per pixel) of Mars, and 2 wide angle cameras, observing in red and blue wavelengths, from which color views of the entire planet are assembled each day. The wide angle cameras provide a daily record of changes in martian weather and surface frost as the seasons progress. MGS MOC has obtained a record of martian weather spanning a little over 2 martian years since it began systematic observations in March 1999.

    The view of Mars shown here was assembled from MOC daily global images obtained on May 12, 2003. At that time, the northern hemisphere was in early autumn, and the southern hemisphere in early spring. At the left/center of this view are the four large Tharsis volcanoes: Olympus Mons, Ascraeus Mons, Pavonis Mons, and Arsia Mons. Stretching across the center of the globe is the 5,000 kilometers (3,000 miles) long Valles Marineris trough system. The seasonal south polar carbon dioxide frost cap is visible at the bottom of this view. A dust storm sweeps across the plains of northern Acidalia at the upper right. North is up, east is right, sunlight illuminates the planet from the left.

  1. Mars surface thermal inertia and heterogeneities from OMEGA/MEX

    NASA Astrophysics Data System (ADS)

    Audouard, J.; Poulet, F.; Vincendon, M.; Bibring, J.-P.; Forget, F.; Langevin, Y.; Gondet, B.

    2014-05-01

    The thermophysical structure of the martian surface is the result of various processes that have shaped the martian surface through time. Previous dedicated heliosynchronous measurements of the thermal infrared (IR) flux of the martian surface have revealed the diversity of martian surface thermal properties, as well as its complexity linked to the heterogeneous nature of terrains. We present the first retrieval of thermophysical properties of the martian surface using near-infrared (NIR) Observatoire pour la Minéralogie, l’Eau, les Glaces et l’Activité (OMEGA) onboard Mars Express (MEX) thermal measurements from 5 to 5.1 μm. MEX orbit around Mars is elliptical and therefore OMEGA has performed surface temperature measurements at various local times and seasons over more than 4 full martian years. We have developed a method to exploit these unprecedented measurements using a one-dimensional energy balance code derived from a Global Climate Model that allows retrieval of the thermal properties of the martian surface using OMEGA data. Regional maps of the thermal inertia at a resolution up to 32 pixels per degree and a global map at 4 pixels per degree are presented. OMEGA-derived thermal inertia values agree with previous mappings by the Thermal Emission Spectrometer (TES) onboard Mars Global Surveyor (MGS) and Thermal Emission Imaging Spectrometer (THEMIS) onboard Mars Odyssey and highlight the key role of dust for the thermal behavior of the martian surface. OMEGA directly reveals for the first time some diurnal variations of apparent TI attributable to surface heterogeneities at macroscopic scale and enables to quantify these heterogeneities. In Nili Patera and Tharsis, local surface heterogeneities are modeled with layering and horizontal admixture of divergent slopes respectively.

  2. Differential Subcellular Localization of Leishmania Alba-Domain Proteins throughout the Parasite Development

    PubMed Central

    Dupé, Aurélien; Dumas, Carole; Papadopoulou, Barbara

    2015-01-01

    Alba-domain proteins are RNA-binding proteins found in archaea and eukaryotes and recently studied in protozoan parasites where they play a role in the regulation of virulence factors and stage-specific proteins. This work describes in silico structural characterization, cellular localization and biochemical analyses of Alba-domain proteins in Leishmania infantum. We show that in contrast to other protozoa, Leishmania have two Alba-domain proteins, LiAlba1 and LiAlba3, representative of the Rpp20- and the Rpp25-like eukaryotic subfamilies, respectively, which share several sequence and structural similarities but also important differences with orthologs in other protozoa, especially in sequences targeted for post-translational modifications. LiAlba1 and LiAlba3 proteins form a complex interacting with other RNA-binding proteins, ribosomal subunits, and translation factors as supported by co-immunoprecipitation and sucrose gradient sedimentation analysis. A higher co-sedimentation of Alba proteins with ribosomal subunits was seen upon conditions of decreased translation, suggesting a role of these proteins in translational repression. The Leishmania Alba-domain proteins display differential cellular localization throughout the parasite development. In the insect promastigote stage, Alba proteins co-localize predominantly to the cytoplasm but they translocate to the nucleolus and the flagellum upon amastigote differentiation in the mammalian host and are found back to the cytoplasm once amastigote differentiation is completed. Heat-shock, a major signal of amastigote differentiation, triggers Alba translocation to the nucleolus and the flagellum. Purification of the Leishmania flagellum confirmed LiAlba3 enrichment in this organelle during amastigote differentiation. Moreover, partial characterization of the Leishmania flagellum proteome of promastigotes and differentiating amastigotes revealed the presence of other RNA-binding proteins, as well as differences in

  3. Mode of antibacterial activity of Eclalbasaponin isolated from Eclipta alba.

    PubMed

    Ray, A; Bharali, P; Konwar, B K

    2013-12-01

    The present study was undertaken to evaluate the mode of antibacterial activity of Eclalbasaponin isolated from Eclipta alba, against selected Gram-positive and Gram-negative bacteria. The probable chemical structure was determined by using various spectroscopic techniques such as Fourier transform infrared spectroscopy (FTIR) and mass spectroscopy. The antibacterial activity was evaluated by well diffusion technique, pH sensitivity, chemotaxis, and crystal violet assays. Eclalbasaponin showed clear zone of inhibition against both Bacillus subtilis and Pseudomonas aeruginosa and exhibited growth inhibition at the pH range of 5.5-9.0. The isolated saponin exhibited its positive chemoattractant property for both bacterial strains. Results of crystal violet assay and the presence of UV-sensitive materials in the cell-free supernatant confirmed the cellular damages caused by the treatment of Eclalbasaponin. The release of intracellular proteins due to the membrane damage was determined by sodium dodecyl sulfate polyacrylamide gel electrophoresis. Changes in the cell surface structure and membrane disruption were further revealed by FTIR and scanning electron microscopy analysis. The present study suggests that the isolated saponin from E. alba causes the disruption of the bacterial cell membrane which leads to the loss of bacterial cell viability.

  4. Lippia alba (Verbenaceae): A new tropical autopolyploid complex?

    PubMed

    Reis, Aryane C; Sousa, Saulo M; Vale, Aline A; Pierre, Patrícia M O; Franco, Ana L; Campos, José Marcello S; Vieira, Roberto F; Viccini, Lyderson F

    2014-06-01

    • Premise of the study: Tropical regions have high species diversity, and polyploidization is a major mechanism of speciation in plants. However, few cases of natural polyploidy have been reported in tropical regions. Lippia alba, is a tropical, aromatic shrub with a wide distribution, extensive morphological plasticity, and several chemotypes. The species has long been recognized as a diploid with 2n = 30 chromosomes. Recently, two variations in chromosome number (2n = 60; 2n = 12-60) have been reported, suggesting the occurrence of polyploidy within the species.• Methods: Flow cytometry was used to investigate the genome size in 106 accessions from 14 Brazilian States. Conventional and molecular cytogenetic techniques and pollen viability analysis were employed to characterize each chromosome number observed.• Key results: The DNA 1C-value varied from 1.17 to 3.45 pg, showing a large variation in genome size. Five distinct chromosome numbers were observed (2n = 30, 38, 45, 60, 90); three are cytogenetically described here for the first time. The 5S rDNA signals varied proportionally according to each chromosome number, but 45S rDNA sites did not. High rates of meiotic irregularity were observed, mainly in cytotypes with higher chromosome numbers.• Conclusions: The data provide new support for the occurrence of a polyploid series in Lippia alba. We provide a hypothesis for how this complex may have arisen. Other cryptic polyploid complexes may remain undiscovered in tropical regions.

  5. Geologic Mapping of MTM -30247, -35247 and -40247 Quadrangles, Reull Vallis Region, Mars

    NASA Technical Reports Server (NTRS)

    Mest, S. C.; Crown, D. A.

    2009-01-01

    Geologic mapping of MTM -30247, -35247, and -40247 quadrangles is being used to characterize Reull Vallis (RV) and to determine the history of the eastern Hellas region of Mars. Studies of RV examine the roles and timing of volatile-driven erosional and depositional processes and provide constraints on potential associated climatic changes. This study complements earlier investigations of the eastern Hellas region, including regional analyses [1-6], mapping studies of circum-Hellas canyons [7-10], and volcanic studies of Hadriaca and Tyrrhena Paterae [11-13]. Key scientific objectives include 1) characterizing RV in its "fluvial zone," 2) analysis of channels in the surrounding plains and potential connections to and interactions with RV, 3) examining young, presumably sedimentary plains along RV, and 4) determining the nature of the connection between the segments of RV.

  6. Geologic Mapping of MTM -30247, -35247 and -40247 Quadrangles, Reull Vallis Region of Mars

    NASA Technical Reports Server (NTRS)

    Mest, S. C.; Crown, D. A.

    2008-01-01

    Geologic mapping and stratigraphic analyses of MTM -30247, -35247, and -40247 quadrangles are being used to characterize the Reull Vallis (RV) system and to determine the history of the eastern Hellas region of Mars. Studies of RV examine the roles and timing of volatile-driven erosional and depositional processes and provide constraints on potential associated climatic changes. This study complements earlier investigations of the eastern Hellas region, including regional analyses [1-6], mapping studies of circum-Hellas canyons [7-10], and volcanic studies of Hadriaca and Tyrrhena Paterae [11-13]. Key scientific objectives for these quadrangles include 1) characterization of RV in its "fluvial zone," 2) analysis of channels in the surrounding plains and potential connections to and interactions with RV, 3) examination of young (?), presumably sedimentary plains along RV that embay the surrounding highlands, and 4) determination of the nature of the connection between segments 1 and 2 of RV.

  7. Feldspathic rocks on Mars: Compositional constraints from infrared spectroscopy and possible formation mechanisms

    NASA Astrophysics Data System (ADS)

    Rogers, A. Deanne; Nekvasil, Hanna

    2015-04-01

    Rare feldspar-dominated surfaces on Mars were previously reported based on near-infrared (NIR) spectral data and were interpreted to consist of anorthosite or felsic rocks. Using thermal infrared (TIR) data over the feldspar detections with the largest areal extent in Nili Patera and Noachis Terra, we rule out felsic interpretations. Basaltic or anorthositic compositions are consistent with TIR measurements, but the geologic contexts for these regions do not support a plutonic origin. Laboratory NIR spectral measurements demonstrate that large plagioclase crystals (>~840 µm) can be detected in mixtures with as much as 50 vol % mafics, which is higher than the previously stated requirement of no more than 15% mafics. Thus, anorthositic or felsic interpretations need not be invoked for all NIR-based feldspar detections. Plagioclase-enriched basaltic eruptive products can be formed from Martian basalts through partial crystallization at the base of a thick crust, followed by low-pressure crystallization of the residual liquids.

  8. Progress in the Scandia Region Geologic Map of Mars

    NASA Technical Reports Server (NTRS)

    Tanaka, K. L.; Rodriguez, J. A. P.

    2010-01-01

    We are in the second year of a four year project to produce a geologic map of the Scandia region of Mars at 1:3,000,000 scale for publication in the USGS Scientific Investigations Map series. The primary objective of the map is to analyze and reconstruct the resurfacing history of this region in much greater detail than achieved by the previous northern plainswide mapping effort. This region includes (1) a broad swath of the Vastitas Borealis plains that includes various Scandia landforms and the Phoenix lander site; (2) part of the margin of the north polar plateau, Planum Boreum; and (3) the northern margin of the immense Alba Mons volcanic shield. We rely mostly on Mars Orbiter Laser Altimeter (MOLA) digital elevation models, Thermal Emission Imaging Spectrometer infrared and visual range, and Context Camera images for mapping and topographic analysis.

  9. Mars habitat

    NASA Technical Reports Server (NTRS)

    Ayers, Dale; Barnes, Timothy; Bryant, Woody; Chowdhury, Parveen; Dillard, Joe; Gardner, Vernadette; Gregory, George; Harmon, Cheryl; Harrell, Brock; Hilton, Sherrill

    1991-01-01

    The objective of this study is to develop a conceptual design for a permanently manned, self-sustaining Martian facility, to accommodate a crew of 20 people. The goal is to incorporate the major functions required for long term habitation in the isolation of a barren planet into a thriving ecosystem. These functions include living, working, service, and medical facilities as well as a green house. The main design task was to focus on the internal layout while investigating the appropriate structure, materials, and construction techniques. The general concept was to create a comfortable, safe living environment for the crew members for a stay of six to twelve months on Mars. Two different concepts were investigated, a modular assembly reusable structure (MARS) designated Lavapolis, and a prefabricated space frame structure called Hexamars. Both models take into account factors such as future expansion, radiation shielding, and ease of assembly.

  10. Mars mission

    NASA Astrophysics Data System (ADS)

    Katzoff, Judith A.

    To mark the 10th anniversary of the Apollo-Soyuz joint space mission, a recent conference examined the prospects for human exploration of Mars and for international cooperation in space. Most of the participants at the conference, which was jointly sponsored by the American Institute of Aeronautics and Astronautics and The Planetary Society, seemed to agree that some sort of collaboration like that between the United States and Soviet Union a decade ago would be desirable, and probably necessary, if humans are ever to reach Mars. Sen. Spark Matsunaga (D-Hawaii) extended the idea by saying that to gain the support of Congress, plans for future space exploration should be tied to international cooperation.

  11. Large-scale volcano-ground ice interactions on Mars

    USGS Publications Warehouse

    Squyres, S. W.; Wilhelms, D.E.; Moosman, A.C.

    1987-01-01

    The process of volcano-ground ice interaction on Mars is investigated by thermodynamic calculations and observations of Viking Orbiter images. We develop a numerical model of volcano-ground ice interaction that includes heat transport by conduction, radiation from the surface, heat transfer to the atmosphere, and H2O phase changes in an ice-rich permafrost. We consider eruption of lava flows over permafrost, and intrusion of sills into permafrost. For eruption of lava over permafrost, most of the heat in the flow is lost by radiation and atmospheric effects. The amount of H2O liquid and vapor produced is small, and its removal would not be sufficient to cause collapse that would lower the surface of the lava flow below the surrounding terrain. For intrusion of a sill, most of the heat in the sill eventually goes into H2O phase changes, producing much larger amounts of water that could have profound geomorphic and geochemical effects. Approximate meltwater discharge rates are calculated for both extrusive and intrusive interactions. We examine two large regions of large-scale volcano-ground ice interactions. Near Aeolis Mensae, intrusion of a complex of dikes and sills into ice-rich ground has produced substantial melting, with mobilization and flow of material. This interaction probably also produced large quantities of palagonite tuff and breccia. Morphologic evidence for progressive fluidization implies that meltwater was stored beneath the surface for some time, and that most of the release of water and volcanic mudflow took place late in the interaction. Northeast of Hellas, several large channels emanate from the area near the volcano Hadriaca Patera. If genetically related to the volcanic activity, large collapse features at the sources of some channels must have originated due to heat from large buried magma bodies. A channel emerging directly from the base of Hadriaca Patera may have originated from release of heat from thick extruded material. Other small

  12. MARS15

    SciTech Connect

    Mokhov, Nikolai

    2016-07-15

    MARS is a Monte Carlo code for inclusive and exclusive simulation of three-dimensional hadronic and electromagnetic cascades, muon, heavy-ion and low-energy neutron transport in accelerator, detector, spacecraft and shielding components in the energy range from a fraction of an electronvolt up to 100 TeV. Recent developments in the MARS15 physical models of hadron, heavy-ion and lepton interactions with nuclei and atoms include a new nuclear cross section library, a model for soft pion production, the cascade-exciton model, the quark gluon string models, deuteron-nucleus and neutrino-nucleus interaction models, detailed description of negative hadron and muon absorption and a unified treatment of muon, charged hadron and heavy-ion electromagnetic interactions with matter. New algorithms are implemented into the code and thoroughly benchmarked against experimental data. The code capabilities to simulate cascades and generate a variety of results in complex media have been also enhanced. Other changes in the current version concern the improved photo- and electro-production of hadrons and muons, improved algorithms for the 3-body decays, particle tracking in magnetic fields, synchrotron radiation by electrons and muons, significantly extended histograming capabilities and material description, and improved computational performance. In addition to direct energy deposition calculations, a new set of fluence-to-dose conversion factors for all particles including neutrino are built into the code. The code includes new modules for calculation of Displacement-per-Atom and nuclide inventory. The powerful ROOT geometry and visualization model implemented in MARS15 provides a large set of geometrical elements with a possibility of producing composite shapes and assemblies and their 3D visualization along with a possible import/export of geometry descriptions created by other codes (via the GDML format) and CAD systems (via the STEP format). The built-in MARS-MAD Beamline

  13. NASA Mars Conference

    SciTech Connect

    Reiber, D.B.

    1988-01-01

    Papers about Mars and Mars exploration are presented, covering topics such as Martian history, geology, volcanism, channels, moons, atmosphere, meteorology, water on the planet, and the possibility of life. The unmanned exploration of Mars is discussed, including the Phobos Mission, the Mars Observer, the Mars Aeronomy Observer, the seismic network, Mars sample return missions, and the Mars Ball, an inflatable-sectored-tire rover concept. Issues dealing with manned exploration of Mars are examined, such as the reasons for exploring Mars, mission scenarios, a transportation system for routine visits, technologies for Mars expeditions, the human factors for Mars missions, life support systems, living and working on Mars, and the report of the National Commission on Space.

  14. Chemical Diversity in Lippia alba (Mill.) N. E. Brown Germplasm

    PubMed Central

    Camêlo, Lídia Cristina Alves; Pinheiro, José Baldin; Andrade, Thiago Matos; Alves, Péricles Barreto

    2015-01-01

    The aim of this study was to perform chemical characterization of Lippia alba accessions from the Active Germplasm Bank of the Federal University of Sergipe. A randomized block experimental design with two replications was applied. The analysis of the chemical composition of the essential oils was conducted using a gas chromatograph coupled to a mass spectrometer. The chemical composition of the essential oils allowed the accessions to be allocated to the following six groups: group 1: linalool, 1,8-cineole, and caryophyllene oxide; group 2: linalool, geranial, neral, 1,8-cineol, and caryophyllene oxide; group 3: limonene, carvone, and sabinene; group 4: carvone, limonene, g-muurolene, and myrcene; group 5: neral, geranial, and caryophyllene oxide; and group 6: geranial, neral, o-cymene, limonene, and caryophyllene oxide. PMID:26075292

  15. Ethnopharmacological Significance of Eclipta alba (L.) Hassk. (Asteraceae)

    PubMed Central

    Jahan, Rownak; Al-Nahain, Abdullah

    2014-01-01

    Eclipta alba can be found growing wild in fallow lands of Bangladesh where it is considered as a weed by farmers. Traditional medicinal systems of the Indian subcontinent countries as well as tribal practitioners consider the plant to have diverse medicinal values and use it commonly for treatment of gastrointestinal disorders, respiratory tract disorders (including asthma), fever, hair loss and graying of hair, liver disorders (including jaundice), skin disorders, spleen enlargement, and cuts and wounds. The plant has several phytoconstituents like wedelolactone, eclalbasaponins, ursolic acid, oleanolic acid, luteolin, and apigenin. Pharmacological activities of plant extracts and individual phytoconstituents have revealed anticancer, hepatoprotective, snake venom neutralizing, anti-inflammatory, and antimicrobial properties. Phytoconstituents like wedelolactone and ursolic and oleanolic acids as well as luteolin and apigenin can form the basis of new drugs against cancer, arthritis, gastrointestinal disorders, skin diseases, and liver disorders. PMID:27355071

  16. Chemical Diversity in Lippia alba (Mill.) N. E. Brown Germplasm.

    PubMed

    Blank, Arie Fitzgerald; Camêlo, Lídia Cristina Alves; Arrigoni-Blank, Maria de Fátima; Pinheiro, José Baldin; Andrade, Thiago Matos; Niculau, Edenilson dos Santos; Alves, Péricles Barreto

    2015-01-01

    The aim of this study was to perform chemical characterization of Lippia alba accessions from the Active Germplasm Bank of the Federal University of Sergipe. A randomized block experimental design with two replications was applied. The analysis of the chemical composition of the essential oils was conducted using a gas chromatograph coupled to a mass spectrometer. The chemical composition of the essential oils allowed the accessions to be allocated to the following six groups: group 1: linalool, 1,8-cineole, and caryophyllene oxide; group 2: linalool, geranial, neral, 1,8-cineol, and caryophyllene oxide; group 3: limonene, carvone, and sabinene; group 4: carvone, limonene, g-muurolene, and myrcene; group 5: neral, geranial, and caryophyllene oxide; and group 6: geranial, neral, o-cymene, limonene, and caryophyllene oxide.

  17. Cytogenetic characterization of Lippia alba and Lantana camara (Verbenaceae) from Brazil.

    PubMed

    Brandão, Aline Dias; Viccini, Lyderson Facio; Salimena, Fátima Regina Gonçalves; Vanzela, André Luiz Laforga; Recco-Pimentel, Shirlei Maria

    2007-03-01

    The aim of this work was to determine the cytogenetic characteristics of Brazilian Lippia alba (Mill) N. E. Brown and Lantana camara Plum. that could be useful for future characterization of these genera. Our analyses revealed that Li. alba has 2n=30 chromosomes consisting of ten metacentric and five submetacentric pairs, while La. camara has 44 metacentric chromosomes. The large blocks of heterochromatin seen in both species suggest an apomorphic condition. Six 45S rDNA sites were detected in both species by fluorescence in situ hybridization (FISH). Two and four 5S rDNA sites were observed in Li. alba and La. camara, respectively. Meiotic analysis revealed a normal chromosomal behaviour. The number of chromosomes and the presence of 45S rDNA and 5S rDNA sites do not exclude a possible polyploid origin. The cytogenetic differences between La. camara and Li. alba may be useful markers for differentiating these species.

  18. Mars @ ASDC

    NASA Astrophysics Data System (ADS)

    Carraro, Francesco

    "Mars @ ASDC" is a project born with the goal of using the new web technologies to assist researches involved in the study of Mars. This project employs Mars map and javascript APIs provided by Google to visualize data acquired by space missions on the planet. So far, visualization of tracks acquired by MARSIS and regions observed by VIRTIS-Rosetta has been implemented. The main reason for the creation of this kind of tool is the difficulty in handling hundreds or thousands of acquisitions, like the ones from MARSIS, and the consequent difficulty in finding observations related to a particular region. This led to the development of a tool which allows to search for acquisitions either by defining the region of interest through a set of geometrical parameters or by manually selecting the region on the map through a few mouse clicks The system allows the visualization of tracks (acquired by MARSIS) or regions (acquired by VIRTIS-Rosetta) which intersect the user defined region. MARSIS tracks can be visualized both in Mercator and polar projections while the regions observed by VIRTIS can presently be visualized only in Mercator projection. The Mercator projection is the standard map provided by Google. The polar projections are provided by NASA and have been developed to be used in combination with APIs provided by Google The whole project has been developed following the "open source" philosophy: the client-side code which handles the functioning of the web page is written in javascript; the server-side code which executes the searches for tracks or regions is written in PHP and the DB which undergoes the system is MySQL.

  19. Mars habitat

    NASA Technical Reports Server (NTRS)

    1991-01-01

    The College of Engineering & Architecture at Prairie View A&M University has been participating in the NASA/USRA Advanced Design Program since 1986. The interdisciplinary nature of the program allowed the involvement of students and faculty throughout the College of Engineering & Architecture for the last five years. The research goal for the 1990-1991 year is to design a human habitat on Mars that can be used as a permanent base for 20 crew members. The research is being conducted by undergraduate students from the Department of Architecture.

  20. Tissue immunostaining for factor XIIIa in dermal dendrocytes of pityriasis alba skin lesions*

    PubMed Central

    Carneiro, Francisca Regina Oliveira; do Amaral, Gabriela Borborema; Mendes, Maiana Darwich; Quaresma, Juarez Antônio Simões

    2014-01-01

    BACKGROUND Pityriasis alba affects 1% of the world population and about 9.9% of the children in Brazil. However, its etiology remains uncertain. OBJECTIVE The objective of the present study was to evaluate the immunoexpression of factor XIIIa in dermal dendrocytes of skin lesions of pityriasis alba. METHOD Twenty patients with pityriasis alba and 20 patients with atopic dermatitis underwent biopsy. The dermal dendrocytes marked by factor XIIIa were counted by means of immunohistochemical analysis. RESULTS The mean amount of dermal dendrocytes found in the patients with pityriasis alba was 2, whereas in the patients with atopic dermatitis it was 4, with a statistically significant difference between them. A cutoff point of 3 cells/square inch was established to differentiate pityriasis alba from atopic dermatitis, with 80% sensibility and 90% specificity. CONCLUSION We believe that pityriasis alba and atopic dermatitis should be considered different clinical forms within the spectrum of atopic disease, in which sun radiation plays an important role by modulating the progression of the disease. PMID:24770500

  1. History of plains resurfacing in the Scandia region of Mars

    USGS Publications Warehouse

    Tanaka, Kenneth L.; Fortezzo, Corey M.; Hayward, Rosalyn K.; Rodriguez, J. Alexis P.; Skinner, James A.

    2011-01-01

    We present a preliminary photogeologic map of the Scandia region of Mars with the objective of reconstructing its resurfacing history. The Scandia region includes the lower section of the regional lowland slope of Vastitas Borealis extending about 500–1800 km away from Alba Mons into the Scandia sub-basin below −4800 m elevation. Twenty mapped geologic units express the diverse stratigraphy of the region. We particularly focus on the materials making up the Vastitas Borealis plains and its Scandia sub-region, where erosional processes have obscured stratigraphic relations and made the reconstruction of the resurfacing history particularly challenging. Geologic mapping implicates the deposition, erosion, and deformation/degradation of geologic units predominantly during Late Hesperian and Early Amazonian time (~3.6–3.3 Ga). During this time, Alba Mons was active, outflow channels were debouching sediments into the northern plains, and basal ice layers of the north polar plateau were accumulating. We identify zones of regional tectonic contraction and extension as well as gradation and mantling. Depressions and scarps within these zones indicate collapse and gradation of Scandia outcrops and surfaces at scales of meters to hundreds of meters. We find that Scandia Tholi display concentric ridges, rugged peaks, irregular depressions, and moats that suggest uplift and tilting of layered plains material by diapirs and extrusion, erosion, and deflation of viscous, sedimentary slurries as previously suggested. These appear to be long-lived features that both pre-date and post-date impact craters. Mesa-forming features may have similar origins and occur along the southern margin of the Scandia region, including near the Phoenix Mars Lander site. Distinctive lobate materials associated with local impact craters suggest impact-induced mobilization of surface materials. We suggest that the formation of the Scandia region features potentially resulted from crustal heating

  2. An integrated model for dune morphology and sand fluxes on Mars

    NASA Astrophysics Data System (ADS)

    Runyon, K. D.; Bridges, N. T.; Ayoub, F.; Newman, C. E.; Quade, J. J.

    2017-01-01

    The transport and deposition of sand is the most prevalent agent of landscape modification on Mars today, with fluxes comparable to some sand dunes on Earth. Until now, the relationship between sand flux and dune field morphology has been poorly constrained. By tracking dune movement over ∼10 km-long dune fields in Herschel Crater and Nili Patera, representative of many dune fields on Mars, we find a downwind flux decrease that correlates with a sequence of changing morphology from barchans to barchanoids and seifs (longitudinal dunes) to isolated dome dunes and ending with sand sheets. We show empirical consistency with atmospheric Internal Boundary Layer (IBL) theory which can describe these broad flux and morphology changes in Martian dune fields. Deviations from IBL flux predictions are from wind streamline compressions up slopes, leading to a speedup effect. By establishing a dune field morphology type example and correlating it with measured and predicted flux changes, we provide an integrated morphology and flux model that can be applied to other areas of Mars and be used to infer paleo-environmental conditions from preserved sandstone.

  3. Mars Exploration Rovers: 4 Years on Mars

    NASA Technical Reports Server (NTRS)

    Landis, Geoffrey A.

    2008-01-01

    This January, the Mars Exploration Rovers "Spirit" and "Opportunity" are starting their fifth year of exploring the surface of Mars, well over ten times their nominal 90-day design lifetime. This lecture discusses the Mars Exploration Rovers, presents the current mission status for the extended mission, some of the most results from the mission and how it is affecting our current view of Mars, and briefly presents the plans for the coming NASA missions to the surface of Mars and concepts for exploration with robots and humans into the next decade, and beyond.

  4. Mars Public Engagement Overview

    NASA Technical Reports Server (NTRS)

    Johnson, Christine

    2009-01-01

    This viewgraph presentation reviews the Mars public engagement goal to understand and protect our home planet, explore the Universe and search for life, and to inspire the next generation of explorers. Teacher workshops, robotics education, Mars student imaging and analysis programs, MARS Student Imaging Project (MSIP), Russian student participation, MARS museum visualization alliance, and commercialization concepts are all addressed in this project.

  5. Plains Style Caldera Complexes: Evidence for Ancient, Explosive Volcanism on Mars

    NASA Astrophysics Data System (ADS)

    Michalski, J. R.; Bleacher, J. E.

    2014-12-01

    One of the mysteries of Mars' geology is the origin of widespread, layered, friable deposits that likely formed through air fall deposition. The enigmatic chaos terrains are largely composed of such deposits, as are many of the most intriguing layered, clay- and sulfate-bearing deposits of astrobiological interest. Such deposits are most likely of volcanic origin, but lack an obvious source, based on comparison with well-known volcanic provinces [1]. We suggest that these deposits may have been sourced from previously unrecognized explosive volcanoes in Arabia Terra. While Arabia is not traditionally considered to be a volcanic region, we propose that several of the large depressions in the area are in fact calderas that formed through a combination of structural collapse and explosive volcanism. These features are characterized by the observation of sets of nested depressions, association with ridged plains, development of ring fractures and faults, the presence of interior slump blocks, and direct association, in some cases, with friable deposits, lavas and evidence for lava lakes. Eden Patera is the type example and shows evidence for three nested calderas with >4000 km3 of collapse volume. Siloe Patera also contains a set of nested collapse features that occur within a zone of demagnetized crust that might indicate the presence of a magma chamber at shallow depth [2]. It is not yet clear why explosive volcanoes may have formed in Arabia Terra, but we suggest that they might represent the rapid rise of mafic magmas through a thin crust. They might represent more silicic or volatile-rich magmas, but these scenarios do not appear to be necessary [3]. We suggest that explosive mafic volcanism was an important aspect of early Martian geological processes. [1] Kerber, L., Head III, J., Madeleine, J. B., Forget, F. & Wilson, L. The dispersal of pyroclasts from ancient explosive volcanoes on Mars: Implications for the friable layered deposits. Icarus 219, 358-381 (2012

  6. Chronology of glaciation in the Hellas region of Mars

    NASA Technical Reports Server (NTRS)

    Johnson, N.; Kargel, Jeffrey S.; Strom, Roger G.; Knight, Christine

    1991-01-01

    The Hellas Impact Basin is one of the oldest features on Mars, as indicated by the high density of large impact craters in parts of the basin. The highly degraded condition of Hellas seems consistent with great antiquity. However, many of the most strikingly modified landscapes in the basin, believed to be glaciogenic, also appear to be geologically youthful. Stratigraphic relations suggest two episodes of glaciation. Chronologic constraints are imposed on glaciation based on the impact cratering record, the focus of which is the southwestern portion of Hellas. Major terrain units are mapped. The lineated terrain and ridged plains form the summit and flanks of a large shield volcano, Amphitrites Patera, which was superimposed over the southwestern rim of Hellas toward the end of heavy bombardment. The ridged plains and lineated terrain are crossed by numerous wrinkle ridges. The lineated terrain is distinguished by a pervasive system of deep erosional troughs and sharp ridges thought to have been glacially sculpted by the Hellas Lobe. It is concluded that glaciation in Hellas occurred during the Middle Amazonian, roughly coeval with glaciation in Argyre.

  7. Radar, visual and thermal characteristics of Mars - Rough planar surfaces

    NASA Technical Reports Server (NTRS)

    Schaber, G. G.

    1980-01-01

    High-resolution Viking Orbiter images contain significant information on Martian surface roughness at 25- to 100-m lateral scales, while earth-based radar observations of Mars are sensitive to roughness at lateral scales of 1 to 30 m or more. High-rms slopes predicted for the Tharsis-Memnonia-Amazonis volcanic plains from extremely weak radar returns are qualitatively confirmed by the Viking image data. Large-scale, curvilinear ridges on lava flows in the Memnonia Fossae region are interpreted as innate flow morphology caused by compressional foldover of moving lava sheets of possible rhyolite-dacite composition. The presence or absence of a recent mantle of fine-grained eolian material on the volcanic surfaces studied was determined by the visibility of fresh impact craters with diameters less than 50 m. Lava flows with surfaces modified by eolian erosion and deposition occur west-northwest of Apollinaris Patera at the border of the cratered equatorial uplands and southern Elysium Planitia. Nearby yardangs, for which radar observations indicate very high-rms slopes, are similar to terrestrial features of similar origin.

  8. MarsSat: assured communication with Mars.

    PubMed

    Gangale, Thomas

    2005-12-01

    The author developed the MarsSat concept during the 1990s. For this task, he designed a class of orbits to solve the problem of communicating with crews on Mars when the planet is in solar conjunction as seen from Earth, a planetary configuration that occurs near the midpoint of a conjunction class mission to Mars. This type of orbit minimizes the distance between Mars and the communications satellite; thus, minimizing the size, weight, and power requirements, while providing a simultaneous line-of-sight to both Earth and Mars. The MarsSat orbits are solar orbits that have the same period as Mars, but are inclined a few degrees out of the plane of the Mars orbit and also differ in eccentricity from the orbit of Mars. These differences cause a spacecraft in this orbit to rise North of Mars, then fall behind Mars, then drop South of Mars, and then pull ahead of Mars, by some desired distance in each case-typically about 20 million kilometers-in order to maintain an angular separation of a couple of degrees as seen from a point in the orbit of Earth on the opposite side of the Sun. A satellite in this type of orbit would relay communications between Earth and Mars during the period of up to several weeks, when direct communication is blocked by the Sun. These orbits are far superior for this purpose when compared to stationing a satellite at one of the Sun-Mars equilateral Lagrangian points, L(4) or L(5), for two reasons. First, L(4) and L(5) are 228 million kilometers from Mars, about 10 times the distance of a spacecraft in one of the MarsSat orbits, and by virtue of the inverse-square law, all other things being equal, the signal strength received at L(4) or L(5) would be one percent of the signal strength received by a spacecraft in one of the MarsSat orbits. Thus, a relay satellite stationed at L(4) or L(5) would have to be that much more powerful to receive data at the same rate, with concomitant increases in spacecraft size and weight. Second, a number of

  9. Multiple paternity in polyandrous barn owls (Tyto alba).

    PubMed

    Henry, Isabelle; Antoniazza, Sylvain; Dubey, Sylvain; Simon, Céline; Waldvogel, Céline; Burri, Reto; Roulin, Alexandre

    2013-01-01

    In polyandrous species females produce successive clutches with several males. Female barn owls (Tyto alba) often desert their offspring and mate to produce a 2(nd) annual brood with a second male. We tested whether copulating during chick rearing at the 1(st) annual brood increases the male's likelihood to obtain paternity at the 2(nd) annual breeding attempt of his female mate in case she deserts their brood to produce a second brood with a different male. Using molecular paternity analyses we found that 2 out of 26 (8%) second annual broods of deserting females contained in total 6 extra-pair young out of 15 nestlings. These young were all sired by the male with whom the female had produced the 1(st) annual brood. In contrast, none of the 49 1(st) annual breeding attempts (219 offspring) and of the 20 2(nd) annual breeding attempts (93 offspring) of non-deserting females contained extra-pair young. We suggest that female desertion can select male counter-strategies to increase paternity and hence individual fitness. Alternatively, females may copulate with the 1(st) male to derive genetic benefits, since he is usually of higher quality than the 2(nd) male which is commonly a yearling individual.

  10. Nanometer accuracy with continuous scans at the ALBA-NOM

    NASA Astrophysics Data System (ADS)

    Nicolas, Josep; Pedreira, Pablo; Å ics, Igors; Ramírez, Claudio; Campos, Juan

    2016-09-01

    We present the continuous scan operation of the ALBA-NOM as a working mode that allows obtaining low noise in short time, as well as high accuracy measurements. In the traditional step-scan operation, the position of the probe beam is kept fixed while many data points of autocollimator are averaged for noise reduction. This operation mode is very safe, as one has a perfect correspondence between mirror position and measured angle, but it is time inefficient, as it disregards all the data values acquired during motion, and basically averages data values taken under identical conditions. On the other hand, continuous scan is less safe in terms of correspondence between mirror position and slope, especially for NOM systems for which the autocollimator does not accept an electronic trigger. Nevertheless, it is possible to perform independent acquisitions of the autocollimator and of the linear stage data during a scan, and synchronize signals a posteriori. This solves the main problem of continuous scan with a NOM. Continuous scan operation for performing measurements is very efficient for noise reduction per unit time, as it allows integrating every single data value taken by the autocollimator. In addition, it opens the possibility of introducing pitch variations of the mirror between scans. This allows obtaining many independent datasets that can be combined using error suppression techniques to reduce not just noise but systematic errors too. In this paper we report the methods and the main results.

  11. Gnathostome infection in swamp eels, Fluta alba, in central Thailand.

    PubMed

    Nuamtanong, S; Waikagul, J; Anantaphruti, M T

    1998-03-01

    To investigate the distribution of gnathostome worms in central Thailand, the infective larvae of Gnathostoma spp were examined from the flesh and liver of swamp eels, Fluta alba. Seven hundred and eighty-eight eels were purchased from markets in 11 provinces; Ang Thong (30), Ayutthaya (36), Chachoengsao (30), Lop Buri (30), Nakhon Nayok (437), Pathum Thani (30), Prachin Buri (48), Ratchaburi (53), Saraburi (30), Samut Prakan (30) and Suphan Buri (34). The highest rate of gnathostome infection was observed in swamp eels from Nakhon Nayok (68.7%). The infection rates in Ayutthaya, Ang Thong, Prachin Buri, Ratchaburi, Saraburi and Lop Buri were 33.3%, 26.7%, 25.0%, 18.9%, 13.3% and 10.0% respectively. Gnathostome larvae were not found in swamp eels from Chachoengsao, Pathum Thani, Samut Prakan and Suphan Buri. Among the 9,573 larvae recovered, almost all were the advanced third stage larvae of G. spinigerum, except one larva from Nakhon Nayok and two larvae from Ratchaburi which were identified as the advanced third stage larvae of G. vietnamicum and G. hispidum respectively. This study is the first report of swamp eels as natural intermediate hosts of G. vietnamicum and G. hispidum.

  12. SimAlba: A Spatial Microsimulation Approach to the Analysis of Health Inequalities.

    PubMed

    Campbell, Malcolm; Ballas, Dimitris

    2016-01-01

    This paper presents applied geographical research based on a spatial microsimulation model, SimAlba, aimed at estimating geographically sensitive health variables in Scotland. SimAlba has been developed in order to answer a variety of "what-if" policy questions pertaining to health policy in Scotland. Using the SimAlba model, it is possible to simulate the distributions of previously unknown variables at the small area level such as smoking, alcohol consumption, mental well-being, and obesity. The SimAlba microdataset has been created by combining Scottish Health Survey and Census data using a deterministic reweighting spatial microsimulation algorithm developed for this purpose. The paper presents SimAlba outputs for Scotland's largest city, Glasgow, and examines the spatial distribution of the simulated variables for small geographical areas in Glasgow as well as the effects on individuals of different policy scenario outcomes. In simulating previously unknown spatial data, a wealth of new perspectives can be examined and explored. This paper explores a small set of those potential avenues of research and shows the power of spatial microsimulation modeling in an urban context.

  13. SimAlba: A Spatial Microsimulation Approach to the Analysis of Health Inequalities

    PubMed Central

    Campbell, Malcolm; Ballas, Dimitris

    2016-01-01

    This paper presents applied geographical research based on a spatial microsimulation model, SimAlba, aimed at estimating geographically sensitive health variables in Scotland. SimAlba has been developed in order to answer a variety of “what-if” policy questions pertaining to health policy in Scotland. Using the SimAlba model, it is possible to simulate the distributions of previously unknown variables at the small area level such as smoking, alcohol consumption, mental well-being, and obesity. The SimAlba microdataset has been created by combining Scottish Health Survey and Census data using a deterministic reweighting spatial microsimulation algorithm developed for this purpose. The paper presents SimAlba outputs for Scotland’s largest city, Glasgow, and examines the spatial distribution of the simulated variables for small geographical areas in Glasgow as well as the effects on individuals of different policy scenario outcomes. In simulating previously unknown spatial data, a wealth of new perspectives can be examined and explored. This paper explores a small set of those potential avenues of research and shows the power of spatial microsimulation modeling in an urban context. PMID:27818989

  14. Investigation of Antiarthritic Potential of Plumeria alba L. Leaves in Acute and Chronic Models of Arthritis

    PubMed Central

    Kumar, Vipin; Gupta, Pankaj; Singh, Surender

    2014-01-01

    Aim. The present investigation was designed to evaluate antiarthritic potential of fractions of hydroalcoholic extract from leaves of P. alba. Materials and Methods. Plumeria alba L. leaves were extracted with hydroalcohol (30 : 70) to obtain hydroalcoholic extract of P. alba. This extract was further fractionated with solvents ethyl acetate and n-butanol to obtain EAPA and BPA, respectively. These fractions were tested against formaldehyde and Freund's complete adjuvant (FCA) induced arthritis. Arthritis assessment, paw volume, body weight, motor incoordination, and nociceptive threshold were measured. On day 21, the animals were sacrificed and histopathology was done. Results. The 100 and 200 mg/kg doses of EAPA and BPA caused a significant (P ≤ 0.05–0.01) reduction in paw swelling in both models. Erythrocyte sedimentation rate (ESR) and spleen weight decreased significantly (P < 0.01) in arthritic rats treated with extracts. There was significant (P < 0.05) improvement in thymus weight in EAPA treated rats whereas significant (P < 0.01) improvement was also seen in haemoglobin level (Hb) in diclofenac treated group. Motor incoordination and nociceptive threshold were also significantly (P ≤ 0.05–0.01) improved. Conclusion. The present study suggests that Plumeria alba L. has protective activity against arthritis and supports the traditional use of P. alba for rheumatism and other inflammatory diseases. PMID:25025056

  15. Immunomodulatory activity of methanolic extract of Morus alba Linn. (mulberry) leaves.

    PubMed

    Bharani, Shendige Eswara Rao; Asad, Mohammed; Dhamanigi, Sunil Samson; Chandrakala, Gowda Kallenahalli

    2010-01-01

    The leaves of Morus alba Linn. (Family: Moraceae) commonly known as mulberry are mainly used as food for the silkworms and they are sometimes eaten as vegetable or used as cattle fodder in different parts of the world. The effect of Morus alba on the immune system was evaluated by using different experimental models such as carbon clearance test, cyclophosphamide induced neutropenia, neutrophil adhesion test, effect on serum immunoglobulins, mice lethality test and indirect haemagglutination test. Methanolic extract of Morus alba was administered orally at low dose and high dose of 100 mg/kg and 1 g/kg respectively and Ocimum sanctum (100 mg/kg, po) was used as standard drug. Morus alba extract in both doses increased the levels of serum immunoglobulins and prevented the mortality induced by bovine Pasteurella multocida in mice. It also increased the circulating antibody titre in indirect haemagglutination test. On the other hand, it showed significant increase in the phagocytic index in carbon clearance assay, a significant protection against cyclophosphamide induced neutropenia and increased the adhesion of neutrophils in the neutrophil adhesion test. Hence, it was concluded that Morus alba increases both humoral immunity and cell mediated immunity.

  16. Identification and effect of two flavonoids from root bark of Morus alba against Ichthyophthirius multifiliis in grass carp

    Technology Transfer Automated Retrieval System (TEKTRAN)

    Morus alba is an important plant for sericulture and has a high medicinal value. In this study, two flavonoids (kuwanons G and O) with antiparasitic activity were isolated from the root bark of M. alba by bioassay-guided fractionation. The chemical structures were determined by pectroscopic analys...

  17. Nicaragua Re-Visited: From Neo-Liberal "Ungovernability" to the Bolivarian Alternative for the Peoples of Our America (ALBA)

    ERIC Educational Resources Information Center

    Muhr, Thomas

    2008-01-01

    In this paper I conduct a historical analysis of the emergence of ALBA in Nicaragua prior to Daniel Ortega's return to the presidency and the country's official membership in the initiative from January 2007 on. I argue that ALBA is a rival structure that evolved from the contradictions inherent in hegemonic globalisation. Within the framework of…

  18. Mars scouts: an overview

    NASA Technical Reports Server (NTRS)

    Matousek, S.

    2001-01-01

    The Mars program institutes the Mars Scout Missions in order to address science goals in the program not otherwise covered in the baseline Mars plan. Mars Scout Missions will be Principle-Investigator (PI) led science missions. Analogous to the Discovery Program, PI led investigations optimize the use of limited resources to accomplish the best focused science and allow the flexibility to quickly respond to discoveries at Mars. Scout missions also require unique investments in technology and reliance upon Mars-based infrastructure such as telecom relay orbiters.

  19. Missions to Mars

    NASA Astrophysics Data System (ADS)

    Chicarro, A. F.; Science Team

    2002-10-01

    This presentation started with a historical perspective of the astronomical discovery of Mars and followed by an overview of previous missions to Mars by the United States and the Soviet Union. Recently launched missions, such as Nozomi, Mars Global Surveyor and Mars Odyssey were addressed in more detailed, as well as a few other missions soon to be launched. Among these, Mars Express is particularly relevant as the first European mission towards the red planet, and the talk concentrated on it, including both the Mars Express orbiter spacecraft and the Beagle-2 lander to be launched in 2003.

  20. Mars integrated transportation system multistage Mars mission

    NASA Technical Reports Server (NTRS)

    1991-01-01

    In accordance with the objective of the Mars Integrated Transport System (MITS) program, the Multistage Mars Mission (MSMM) design team developed a profile for a manned mission to Mars. The purpose of the multistage mission is to send a crew of five astronauts to the martian surface by the year 2019. The mission continues man's eternal quest for exploration of new frontiers. This mission has a scheduled duration of 426 days that includes experimentation en route as well as surface exploration and experimentation. The MSMM is also designed as a foundation for a continuing program leading to the colonization of the planet Mars.

  1. New microsatellite loci for Prosopis alba and P. chilensis (Fabaceae)1

    PubMed Central

    Bessega, Cecilia F.; Pometti, Carolina L.; Miller, Joe T.; Watts, Richard; Saidman, Beatriz O.; Vilardi, Juan C.

    2013-01-01

    • Premise of the study: As only six useful microsatellite loci that exhibit broad cross-amplification are so far available for Prosopis species, it is necessary to develop a larger number of codominant markers for population genetic studies. Simple sequence repeat (SSR) markers obtained for Prosopis species from a 454 pyrosequencing run were optimized and characterized for studies in P. alba and P. chilensis. • Methods and Results: Twelve markers that were successfully amplified showed polymorphism in P. alba and P. chilensis. The number of alleles per locus ranged between two and seven and heterozygosity estimates ranged from 0.2 to 0.8. Most of these loci cross-amplify in P. ruscifolia, P. flexuosa, P. kuntzei, P. glandulosa, and P. pallida. • Conclusions: These loci will enable genetic diversity studies of P. alba and P. chilensis and contribute to fine-scale population structure, indirect estimation of relatedness among individuals, and marker-assisted selection. PMID:25202541

  2. Flour from Prosopis alba cotyledons: A natural source of nutrient and bioactive phytochemicals.

    PubMed

    Cattaneo, F; Costamagna, M S; Zampini, I C; Sayago, J; Alberto, M R; Chamorro, V; Pazos, A; Thomas-Valdés, S; Schmeda-Hirschmann, G; Isla, M I

    2016-10-01

    The Prosopis alba seed is a waste material in the process to produce pod flour. To suggest a potential use of these seeds it is necessary to determine the nutritional, phytochemical and functional quality of cotyledon flour from Prosopis alba. This flour showed high level of proteins (62%), low content of total carbohydrate and fat. Free polyphenol (1150±20mg GAE/100g flour) and carotenoids (10.55±0.05mg β-CE/100g flour) compounds were the dominant compounds. The main identified constituents in the polyphenolic extracts were C- glycosyl flavones, including schaftoside, isoschaftoside, vicenin II, vitexin and isovitexin. The extract enriched in polyphenolic compounds exhibited ABTS(+) reducing capacity and scavenging activity of H2O2; and was able to inhibit phospholipase, lipoxygenase and cyclooxygenase, three pro-inflammatory enzymes. According to our results, the P. alba cotyledon flour could be considered as a new alternative in the formulation of functional foods or food supplements.

  3. Effect of Morus alba L. (mulberry) leaves on anxiety in mice

    PubMed Central

    Yadav, A.V.; Kawale, L.A.; Nade, V.S.

    2008-01-01

    Objective: The aim of the present work is to evaluate the anxiolytic effect of a methanolic extract of Morus alba L. leaves in mice. Materials and Methods: The hole-board test, elevated plus-maze paradigm, open field test, and light/dark paradigm were used to assess the anxiolytic activity of the methanolic extract of M. alba L. Morus alba extract (50, 100, and 200 mg/kg, i.p.) and diazepam (1 mg/kg, i.p.) were administered 30 min before the tests. Results: The results showed that the methanolic extract of M. alba significantly increased the number and duration of head poking in the hole-board test. In the elevated plus-maze, the extract significantly increased the exploration of the open arm in similar way to that of diazepam. At a dose of 200 mg/kg i.p. the extract significantly increased both the time spent in and the entries into the open arm by mice. Further, in the open field test, the extract significantly increased rearing, assisted rearing, and number of squares traversed, all of which are demonstrations of exploratory behavior. In the light/dark paradigm, the extract produced significant increase in time spent in the lighted box as compared to vehicle. The spontaneous locomotor activity count, measured using an actophotometer, was significantly decreased in animals pretreated with M. alba extract, indicating a remarkable sedative effect of the plant. Conclusion: The results of the present study suggest that a methanolic extract of M. alba leaves may possess an anxiolytic effect. PMID:21264159

  4. Purification and biochemical characterization of phytocystatin from Brassica alba.

    PubMed

    Ahmed, Azaj; Shamsi, Anas; Bano, Bilqees

    2016-05-01

    Phytocystatins belong to the family of cysteine proteinases inhibitors. They are ubiquitously found in plants and carry out various significant physiological functions. These plant derived inhibitors are gaining wide consideration as potential candidate in engineering transgenic crops and in drug designing. Hence it is crucial to identify these inhibitors from various plant sources. In the present study a phytocystatin has been isolated and purified by a simple two-step procedure using ammonium sulfate saturation and gel filtration chromatography on Sephacryl S-100HR from Brassica alba seeds (yellow mustard seeds).The protein was purified to homogeneity with 60.3% yield and 180-fold of purification. The molecular mass of the mustard seed cystatin was estimated to be nearly 26,000 Da by sodium dodecyl sulfate polyacrylamide gel electrophoresis as well as by gel filtration chromatography. The stokes radius and diffusion coefficient of the mustard cystatin were found to be 23A° and 9.4 × 10(-7)  cm(2) s(-1) respectively. The isolated phytocystatin was found to be stable in the pH range of 6-8 and is thermostable up to 60 °C. Kinetic analysis revealed that the phytocystatin exhibited non-competitive type of inhibition and inhibited papain more efficiently (K(i)  = 3 × 10(-7)  M) than ficin (K(i)  = 6.6 × 10(-7)  M) and bromelain (K(i) = 7.7 × 10(-7)  M respectively). CD spectral analysis shows that it possesses 17.11% alpha helical content.

  5. Possibilities of Terraforming Mars

    NASA Astrophysics Data System (ADS)

    Shrivastava, M. K.

    2007-07-01

    Diminished internally produced energy of early Mars would have resulted in cold mantle, causing gradual submersion of surface water with dissolved gases. Therefore, to terraform or revive Mars, it is necessary to reactivate its diminished internally produced energy.

  6. MAVEN's Trajectory to Mars

    NASA Video Gallery

    This movie shows the cruise trajectory of NASA's Mars Atmosphere and Volatile Evolution (MAVEN) mission, which was launched on Nov. 18, 2013. It will arrive at Mars on Sept. 21, 2014, to explore th...

  7. Mars Meteorolgical Network

    NASA Technical Reports Server (NTRS)

    Justh, H. L.; Spann, J. F.

    2012-01-01

    Exploring and ultimately establishing a permanent presence on the surface of Mars will necessitate an understanding the weather conditions and the ability to forecast its dynamic behavior. The meteorology of Mars will need to be developed. This abstract puts forth a concept for a Mars Meteorological Network that will be used to investigate the Mars atmosphere behavior, explore the surface environment, and prepare for operational activities. It is proposed that the long term and the dynamic nature of the lower atmosphere and surface of Mars be observed with a distributed global array of simple automated surface nodes. The data would be ingested into the Mars Global Reference Atmospheric Model (Mars-GRAM) and other research tools for analyses to gain a better understanding of the atmospheric conditions on Mars.

  8. The Mars Chamber

    NASA Video Gallery

    The Mars chamber is a box about the size of a refrigerator that re-creates the temperatures, pressures, and atmosphere of the Martian surface, essentially creating a Mars environment on Earth! Scie...

  9. Mars - Water Ice Clouds

    NASA Technical Reports Server (NTRS)

    1997-01-01

    The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO.

  10. Rotorcrafts for Mars Exploration

    NASA Astrophysics Data System (ADS)

    Balaram, J.; Tokumaru, P. T.

    2014-06-01

    Rotorcraft mobility provides a number of useful capabilities to potential Mars missions. We present some recent results relating to the design and test of Mars rotorcraft mobility elements, and aspects of rotorcraft system and mission design.

  11. Antioxidant and neurosedative properties of polyphenols and iridoids from Lippia alba.

    PubMed

    Hennebelle, Thierry; Sahpaz, Sevser; Gressier, Bernard; Joseph, Henry; Bailleul, François

    2008-02-01

    The neurosedative and antioxidative properties of some major compounds isolated from a citral chemotype of Lippia alba were investigated. Binding assays were performed on two CNS inhibitory targets: benzodiazepine and GABA(A) receptors. The most active compound was luteolin-7-diglucuronide, with half maximal inhibitory concentrations (IC(50)) of 101 and 40 microm, respectively. Fifteen compounds isolated from Lippia alba were tested for their radical scavenging capacities against DPPH. Four of the major compounds (verbascoside, calceolarioside E, luteolin-7-diglucuronide and theveside) were also tested for their antioxidant activity against superoxide radical-anion in cell-free (hypoxanthine-xanthine oxidase) and cellular (PMA-stimulated neutrophil granulocytes) systems.

  12. Anaerobic reduction of elemental sulfur by Chromatium vinosum and Beggiatoa alba

    NASA Technical Reports Server (NTRS)

    Schmidt, T. M.

    1985-01-01

    The effect of sulfur globules on the buoyant density of Chromatium vinosum and Beggiatoa alba was examined. The potential use of sulfur as a terminal electron acceptor in the anaerobic metabolism of Beggiatoa alba is also examined. The effect of the reduction of intracellular sulfur was investigated during dark metabolism on the buoyant density of C. vinosum. It is hypothesized from the results that the sulfur reduction to sulfide is part of an anaerobic energy operating system. Carbon stored as PHB can be oxidized with the concomitant reduction of sulfur to sulfide.

  13. True Colors of Mars

    NASA Technical Reports Server (NTRS)

    2004-01-01

    This image taken on Mars by the panoramic camera on the Mars Exploration Rover Spirit shows the rover's color calibration target, also known as the MarsDial. The target's mirror and the shadows cast on it by the Sun help scientists determine the degree to which dusty martian skies alter the panoramic camera's perception of color. By adjusting for this effect, Mars can be seen in all its true colors.

  14. Rotorcraft as Mars Scouts

    NASA Technical Reports Server (NTRS)

    Young, L. A.; Aiken, E. W.; Gulick, V.; Mancinelli, R.; Briggs, G. A.; Rutkowski, Michael (Technical Monitor)

    2002-01-01

    A new approach for the robotic exploration of Mars is detailed in this paper: the use of small, ultralightweight, autonomous rotary-wing aerial platforms. Missions based on robotic rotorcraft could make excellent candidates for NASA Mars Scout program. The paper details the work to date and future planning required for the development of such 'Mars rotorcraft.'

  15. 1 Main Street, Mars

    NASA Technical Reports Server (NTRS)

    1997-01-01

    Located outside StenniSphere, the visitor center at John C. Stennis Space Center, 1 Main Street Mars is a model of how a habitat on Mars might look. Complete with thermometers, scales and clocks set to Martian equivalents, this exhibit shows how very different life on Mars can be.

  16. Tectonic Evolution of Mars

    NASA Technical Reports Server (NTRS)

    Phillips, Roger J.

    1992-01-01

    The Final Technical Report on tectonic evolution of Mars is presented. Two papers and an abstract are included. Topics addressed include: scientific rationale and requirements for a global seismic network on Mars, permanent uplift in magmatic systems with application to the Tharsis Region of Mars, and the geophysical signal of the Martian global dichotomy.

  17. Bedform Migration on Mars: Current Results, Implications, and Future Plans

    NASA Astrophysics Data System (ADS)

    Bridges, N. T.; Avouac, J.; Ayoub, F.; Banks, M. E.; Geissler, P. E.; Leprince, S.; Lucas, A.; Mattson, S.; Silvestro, S.

    2012-12-01

    Mars contains a diversity of aeolian bedforms, many with characteristics like those found on Earth. Prior to MRO, studies were largely focused on the distribution, morphology, and sediment pathways of dunes. With the higher resolution provided by HiRISE, detailed measurements of ripple and dune migration, and derivation of sand flux and abrasion rates, are possible. Of 88 image pairs examined from 77°S to 86°N, 42 (48%) exhibit no detectable change (that is, down to ~3 pixels, or 0.75-0.9 m), 36 (41%) show bedform migration, and 10 (11%) are inconclusive. Migration rates range from the limit of resolution to 12 m per Earth year. Martian dunes and ripples migrate over diverse areas of the planet, with the north polar erg the most prevalent geographic region for displacement. Active bedforms tend to have dark tones and crisp textures, with inactive features commonly lighter in tone and many having ridge-like morphologies. As of yet, no geographic, latitudinal, topographic, or albedo correlations, nor any linkage to results from global circulation models, have come from the analyzed data. Rather, migration may be tied to very local conditions where a sufficient frequency of gusts initiates saltation, which is then sustained by the low impact thresholds on Mars. Sub-pixel registration and correlation using COSI-Corr can quantitatively measure displacements over an entire scene down to scales of 1/3 of a pixel or less (so ~≤ 8 cm). Using these techniques, sand fluxes have been derived for the Nili Patera dune field. Fluxes between Ls = 268° to 330° (northern winter) are ~2.3 m3 m-1 yr-1. These values, and estimated rock abrasion rates of 1-50 μm yr-1, are equivalent to those estimated in Victoria Valley, Antarctica. The reptation/saltation flux is found at ~5, similar to results on Earth. Examining Nili images at other dates shows that flux correlates to the seasonal changes in pressure as measured by surface meteorology stations, indicating a lowering of the

  18. Threshold for sand mobility on Mars calibrated from seasonal variations of sand flux.

    PubMed

    Ayoub, F; Avouac, J-P; Newman, C E; Richardson, M I; Lucas, A; Leprince, S; Bridges, N T

    2014-09-30

    Coupling between surface winds and saltation is a fundamental factor governing geological activity and climate on Mars. Saltation of sand is crucial for both erosion of the surface and dust lifting into the atmosphere. Wind tunnel experiments along with measurements from surface meteorology stations and modelling of wind speeds suggest that winds should only rarely move sand on Mars. However, evidence for currently active dune migration has recently accumulated. Crucially, the frequency of sand-moving events and the implied threshold wind stresses for saltation have remained unknown. Here we present detailed measurements of Nili Patera dune field based on High Resolution Imaging Science Experiment images, demonstrating that sand motion occurs daily throughout much of the year and that the resulting sand flux is strongly seasonal. Analysis of the seasonal sand flux variation suggests an effective threshold for sand motion for application to large-scale model wind fields (1-100 km scale) of τ(s)=0.01±0.0015 N m(-2).

  19. Geologic Map of the Hellas Region of Mars

    USGS Publications Warehouse

    Leonard, Gregory J.; Tanaka, Kenneth L.

    2001-01-01

    INTRODUCTION This geologic map of the Hellas region focuses on the stratigraphic, structural, and erosional histories associated with the largest well-preserved impact basin on Mars. Along with the uplifted rim and huge, partly infilled inner basin (Hellas Planitia) of the Hellas basin impact structure, the map region includes areas of ancient highland terrain, broad volcanic edifices and deposits, and extensive channels. Geologic activity recorded in the region spans all major epochs of martian chronology, from the early formation of the impact basin to ongoing resurfacing caused by eolian activity. The Hellas region, whose name refers to the classical term for Greece, has been known from telescopic observations as a prominent bright feature on the surface of Mars for more than a century (see Blunck, 1982). More recently, spacecraft imaging has greatly improved our visual perception of Mars and made possible its geologic interpretation. Here, our mapping at 1:5,000,000 scale is based on images obtained by the Viking Orbiters, which produced higher quality images than their predecessor, Mariner 9. Previous geologic maps of the region include those of the 1:5,000,000-scale global series based on Mariner 9 images (Potter, 1976; Peterson, 1977; King, 1978); the 1:15,000,000-scale global series based on Viking images (Greeley and Guest, 1987; Tanaka and Scott, 1987); and detailed 1:500,000-scale maps of Tyrrhena Patera (Gregg and others, 1998), Dao, Harmakhis, and Reull Valles (Price, 1998; Mest and Crown, in press), Hadriaca Patera (D.A. Crown and R. Greeley, map in preparation), and western Hellas Planitia (J.M. Moore and D.E. Wilhelms, map in preparation). We incorporated some of the previous work, but our map differs markedly in the identification and organization of map units. For example, we divide the Hellas assemblage of Greeley and Guest (1987) into the Hellas Planitia and Hellas rim assemblages and change the way units within these groupings are identified

  20. Channel geometry and discharge estimates for Dao and Niger Valles, Mars

    NASA Astrophysics Data System (ADS)

    Musiol, S.; van Gasselt, S.; Neukum, G.

    2008-09-01

    Introduction The outflow channels Dao and Niger Valles are located at the eastern rim of the 2000-km diameter Hellas Planitia impact basin, in a transition zone with ancient cratered terrain and the volcanoes Hadriaca and Tyrrhena Patera (Hesperia Planum) on the one hand and fluvial, mass-wasting and aeolian deposits on the other hand [1]. Dao and Niger have alcove-shaped source regions similar to the chaotic terrains found in the Margaritifer Terra region, with flat floors, landslide morphologies and small, chaotically distributed isolated mounds. As [2] pointed out, the intrusion of volcanic material could be responsible for the release of pressurized water that can carry loose material away. This process could than have created a depression and an associated outflow channel. In contrast to [2] who made their calculations for Aromatum Chaos and Ravi Vallis, we have focused on Dao and Niger Valles for investigation, since they are spatially related to the nearby Hadriaca Patera. Heat-triggered outflow events seem likely. We follow the generally accepted assumption that water was the main erosional agent [3]. Furthermore we take into account that multiple floods with different volumes are more likely than a single event because of repressurization of an aquifer [4]. Background Hadriaca Patera Hadriaca Patera is among the oldest central-vent volcanoes on Mars, a low-relief volcano with a central caldera complex which consists predominantly of pyroclastic material. The erosional structure of degraded valleys on its flanks is indicative of dissection by a combination of groundwater sapping and surface runoff, attributed to a hydromagmatic eruption scenario [5]. Dao Vallis Dao Vallis is interpreted as collapse region of volcanic and sedimentary plains that have been eroded by surface and subsurface flow [5]. The approximately radial alignment to Hellas is interpreted as following deep-seated structural weakness zones generated by the impact. Small grabens and fractures

  1. Are sinuous ridges in the equatorial Rahway Vallis region of Mars fluvioglacial in origin?

    NASA Astrophysics Data System (ADS)

    Ramsdale, Jason D.; Balme, Matt R.; Conway, Susan J.; Gallagher, Colman

    2013-04-01

    A suite of elongate, branching positive relief landforms has been observed around Rahway Vallis, south-west of Orcus Patera, Mars. They are typically 10 to 150 metres across, and several to tens of kilometres in length. We have observed that these forms occur both individually and as part of complex systems incorporating various cross-cutting, anastomosing and branching patterns. This study forms part of a larger debate as to whether fluvioglacial processes, as opposed to igneous activity, shaped the landscapes in the Elysium Planitia region. The similarity of some of these positive relief branching forms to inverted channels, or perhaps even relict sub-glacial fluvial systems (eskers) suggests an alternative fluvioglacial hypothesis to formation by volcanic processes. Interestingly, if these are esker-like forms then glacial activity in this region was "wet-based", so there should be other characteristic landforms visible. To address this idea, we are conducting a new mapping study of sinuous ridges in the region around Rahway Vallis to assess whether they are more consistent in morphology with formation by igneous or fluvioglacial processes. The survey is being performed using orbital images from the Context Camera (CTX) on the Mars Reconnaissance Orbiter and elevation data from the Mars Orbiter Laser Altimeter (MOLA). Our mapping has shown that many of the ridges form convergent, contributory networks. The ridges are spatially associated with kilometre-wide shallow channels and are found at a nearly constant elevation of -3000m above Mars Datum. Our preliminary interpretation is that these ridges are depositional landforms with multiple sources, and therefore could be sub-glacial (eskers), or inverted fluvial channels. The associated larger channels could be higher order fluvial channels, with the ridges and wide-channels together forming part of a larger drainage network.

  2. Mars Drilling Status

    NASA Technical Reports Server (NTRS)

    Mandell, Humboldt, C., Jr.

    2002-01-01

    This slide presentation reviews the current status of work to explore Mars beneath the surface of planet. One of the objective of this work is to enable further exploration of Mars by humans. One of the requirements for this is to find water on Mars. The presences of water is critical for Human Exploration and a permanent presence on Mars. If water is present beneath the surface it is the best chance of finding life on Mars. The presentation includes a timeline showing the robotic missions, those that have already been on Mars, and planned missions, an explanation of why do we want to drill on Mars, and some of the challenges, Also include are reviews of a missions that would drill 200 and 4,000 to 6,000 meters into the Martian bedrock, and a overview description of the drill. There is a view of some places where we have hopes of finding water.

  3. Solar Power on Mars

    NASA Technical Reports Server (NTRS)

    2005-01-01

    This chart illustrates the variation in available solar power for each of NASA's twin Mars Exploration Rovers over the course of approximately two Mars years. Two factors affect the amount of available power: the tilt of Mars' axis and the eccentricity of the Mars' orbit about the sun.

    The horizontal scale is the number of Martian days (sols) after the Jan. 4, 2004, (Universal Time) landing of Spirit at Mars' Gusev Crater. The vertical scale on the right indicates the amount of available solar power as a ratio of the amount available at the equator when Mars is closest to the sun (perihelion). The red line indicates power availability at Spirit's landing site (Gusev). The blue line indicates power availability at Opportunity's landing site (Meridiani).

    The vertical scale on the right applies to the dotted line, indicating the latitude north or south of Mars' equator where the noon sun is overhead at different times of the Martian year.

  4. Alcoholic Extract of Eclipta alba Shows In Vitro Antioxidant and Anticancer Activity without Exhibiting Toxicological Effects

    PubMed Central

    Arya, Rakesh Kumar; Dev, Kapil; Sharma, Chetan; Hossain, Zakir; Meena, Sanjeev; Arya, K. R.; Gayen, J. R.

    2017-01-01

    As per WHO estimates, 80% of people around the world use medicinal plants for the cure and prevention of various diseases including cancer owing to their easy availability and cost effectiveness. Eclipta alba has long been used in Ayurveda to treat liver diseases, eye ailments, and hair related disorders. The promising medicinal value of E. alba prompted us to study the antioxidant, nontoxic, and anticancer potential of its alcoholic extract. In the current study, we evaluated the in vitro cytotoxic and antioxidant effect of the alcoholic extract of Eclipta alba (AEEA) in multiple cancer cell lines along with control. We have also evaluated its effect on different in vivo toxicity parameters. Here, we found that AEEA was found to be most active in most of the cancer cell lines but it significantly induced apoptosis in human breast cancer cell lines by disrupting mitochondrial membrane potential and DNA damage. Moreover, AEEA treatment inhibited migration in both MCF 7 and MDA-MB-231 cells in a dose dependent manner. Further, AEEA possesses robust in vitro antioxidant activity along with high total phenolic and flavonoid contents. In summary, our results indicate that Eclipta alba has enormous potential in complementary and alternative medicine for the treatment of cancer. PMID:28250894

  5. BBC ALBA's Contributions to Gaelic Language Planning Efforts for Reversing Language Shift

    ERIC Educational Resources Information Center

    Milligan, Lindsay; Chalmers, Douglas; Danson, Mike; Lang, Alison

    2011-01-01

    BBC ALBA is the first dedicated Gaelic-medium television channel in history. It launched in September 2008 and, in late 2010, announced that it would be carried on Freeview, in addition to Sky, Freesat, and BBC iPlayer, thereby widening access to Gaelic throughout Scotland. The channel is a BBC-licensed service that is presently operated as a…

  6. Chemical characterization of Lippia alba essential oil: an alternative to control green molds

    PubMed Central

    Glamočlija, Jasmina; Soković, Marina; Tešević, Vele; Linde, Giani Andrea; Colauto, Nelson Barros

    2011-01-01

    The essential oil of Lippia alba is reported as an antifungal against human pathogenic microorganisms but few articles report its use as an alternative to synthetic fungicides on green mould control. The objective of this study was to determine chemical characteristics of L. alba essential oil and its antifungal activity against green molds as an alternative to synthetic fungicides. Essential oil was extracted by Clevenger hydrodistillation, characterized by GC-MS analysis, and the structure of the main compounds confirmed by 1H and 13C-NMR spectroscopy. Microdilution assays evaluated the essential oil minimum inhibitory concentration (MIC) and minimum fungicidal concentration (MFC). Commercial fungicides Ketoconazole and Bifonazole were used as control. Essential oil yield is of 0.15% and the major components are neral (33.32%) and geranial (50.94%). The L. alba essential oil has MIC of 0.300–1.250 mg/mL and MFC of 0.600–1.250 mg/mL. Ketoconazole and Bifonazole show MIC ranging from 0.025–0.500 to 0.100–0.200 mg/mL, and MFC ranging from 0.250–0.100 to 0.200–0.250 mg/mL, respectively. L. alba essential oil is classified as citral type and the results indicate that it is a potential alternative to synthetic fungicides. PMID:24031788

  7. Pacific Northwest Condiment Yellow Mustard (Sinapis alba L.) Grower Guide: 2000-2002

    SciTech Connect

    Brown, J.; Davis, J. B.; Esser, A.

    2005-07-01

    This report is a grower guide for yellow mustard. Yellow mustard (Sinapis alba L.), synonymous with white mustard, is a spring annual crop and well adapted to hot, dry growing conditions. It has shown potential as an alternative crop in rotations with small grain cereals and has fewer limitations compared to other traditional alternative crops.

  8. Analysis of the biosynthesis of antibacterial cyclic dipeptides in Nocardiopsis alba.

    PubMed

    Li, Yongli; Lai, Ying-Mi; Lu, Yi; Yang, Yu-Liang; Chen, Shawn

    2014-11-01

    Nocardiopsis alba is frequently isolated from environment and has recently been suggested as a casual symbiotic actinobacterium of diverse invertebrates. Using activity-guided fractionation, we purified two antibacterial cyclic dipeptides, cyclo(ΔPhe-ΔLeu) (albonoursin) and cyclo(ΔmTyr-ΔLeu), from a culture of Nocardiopsis alba ATCC BAA-2165. Analysis of N. alba genome revealed genetic information similar to albonoursin biosynthetic gene cluster, albABC. An albABC gene deletion mutant of N. alba was generated. Liquid chromatography-mass spectrometry analysis showed that the mutant could not produce the cyclic dipeptides. Cyclic dipeptide production in the mutant was restored by genetic complementation with the albABC cloned in a native plasmid of Nocardiopsis. β-Glucuronidase reporter assays with a second mutant construct, in which albABC promoter is transcriptionally fused to the reporting gene gusA, indicated that albABC gene expression was subject to osmoregulation. The system presented will be used to study the metabolic and genetic control of cyclic dipeptide biosynthesis in Nocardiopsis.

  9. Essential oils and isolated compounds from Lippia alba leaves and flowers: antimicrobial activity and osteoclast apoptosis.

    PubMed

    Juiz, Paulo José Lima; Lucchese, Angelica Maria; Gambari, Roberto; Piva, Roberta; Penolazzi, Letizia; Di Ciano, Martina; Uetanabaro, Ana Paula Trovatti; Silva, Franceli; Avila-Campos, Mario Julio

    2015-01-01

    In the present study, essential oils extracted from the leaves and flowers of Lippia alba (Mill.) N.E.Br. (L. alba) were analyzed for their antimicrobial activity and their effects on osteoclasts. The periodontal pathogens, Aggregatibacter actinomycetemcomitans (A. actinomycetemcomitans; ATCC 43717), Fusobacterium nucleatum (F. nucleatum; ATCC 25586) and Porphyromonas gingivalis (P. gingivalis); ATCC 33277) were used in antimicrobial activity assays for determining the minimum inhibitory concentration (MIC) and the minimum bactericidal concentration (MBC), whereas Bacteroides fragilis (B. fragilis; ATCC 25285) was used as the control microorganism. Osteoclast (OC) apoptosis was assessed by TUNEL assay and Fas receptor expression was detected by immunocytochemistry. The analysis of antimicrobial activity revealed that P. gingivalis had the lowest MIC values, whereas A. actinomycetemcomitans had the highest. L. alba essential oils were found to be toxic to human cells, although the compounds, carvone, limonene and citral, were non-toxic and induced apoptosis in the OCs. This study demonstrates that L. alba has potential biotechnological application in dentistry. In fact periodontal disease has a multifactorial etiology, and the immune response to microbial challenge leads to osteoclast activation and the resorption of the alveolar bone, resulting in tooth loss.

  10. [Genetic control of Silver fir isozymes (Abies alba Mill.) of the Ukrainian Carpathian Mountains].

    PubMed

    Korshikov, I I; Morozova, N N; Pirko, Ia V

    2003-01-01

    Genetic control of GOT, GDH, DIA, MDH, ME, SOD, FDH, ADH, ACP, LAP enzymes has been studied in the seed megagametophytes of Silver fir (Abies alba Mill.) from four natural populations of the Ukrainian Carpathian mountains. The distinct electrophoretic division has been obtained for the 21 loci products. The analysis of allele segregation in the heterozygous trees confirms monogenic inheritance of the revealed variants.

  11. Chemical characterization of Lippia alba essential oil: an alternative to control green molds.

    PubMed

    Glamočlija, Jasmina; Soković, Marina; Tešević, Vele; Linde, Giani Andrea; Colauto, Nelson Barros

    2011-10-01

    The essential oil of Lippia alba is reported as an antifungal against human pathogenic microorganisms but few articles report its use as an alternative to synthetic fungicides on green mould control. The objective of this study was to determine chemical characteristics of L. alba essential oil and its antifungal activity against green molds as an alternative to synthetic fungicides. Essential oil was extracted by Clevenger hydrodistillation, characterized by GC-MS analysis, and the structure of the main compounds confirmed by (1)H and (13)C-NMR spectroscopy. Microdilution assays evaluated the essential oil minimum inhibitory concentration (MIC) and minimum fungicidal concentration (MFC). Commercial fungicides Ketoconazole and Bifonazole were used as control. Essential oil yield is of 0.15% and the major components are neral (33.32%) and geranial (50.94%). The L. alba essential oil has MIC of 0.300-1.250 mg/mL and MFC of 0.600-1.250 mg/mL. Ketoconazole and Bifonazole show MIC ranging from 0.025-0.500 to 0.100-0.200 mg/mL, and MFC ranging from 0.250-0.100 to 0.200-0.250 mg/mL, respectively. L. alba essential oil is classified as citral type and the results indicate that it is a potential alternative to synthetic fungicides.

  12. Activity of meadowfoam (Limnanthes alba) seed meal glucolimnanthin degradation products against soilborne pathogens

    Technology Transfer Automated Retrieval System (TEKTRAN)

    Meadowfoam (Limnanthes alba L.) is a herbaceous winter-spring annual grown as a commercial oilseed crop. The meal remaining after oil extraction from the seed contains up to 4% of the glucosinolate glucolimnanthin. Degradation of glucolimnanthin yields toxic breakdown products, and therefore the mea...

  13. Rejoinder: On the Dangers of Rosy Lenses--"Reply to Alba, Kasinitz and Waters"

    ERIC Educational Resources Information Center

    Haller, William; Portes, Alejandro; Lynch, Scott M.

    2011-01-01

    We commend the measured tone and clearly stated arguments in Alba, Kasinitz and Waters' commentary on our article. It is particularly welcome because, in combination with our own conclusions, it lays out before the relevant audiences the substance of the debate in this field. Based on the commentary's opening statement, it would appear that there…

  14. [In vitro evaluation of antileishmania activity of Artemisia herba alba Asso].

    PubMed

    Hatimi, S; Boudouma, M; Bichichi, M; Chaib, N; Idrissi, N G

    2001-03-01

    Aqueous extract and essential oil of Artemisia herba-alba Asso were tested for their antileshmanial activity again Leishmania tropica and Leishmania major. The strongest leishmanicidal activity was observed with the essential oil at 2 micrograms/ml as versus the other two strains tested. The aqueous extract showed an antileshmanial activity at 4 micrograms/ml.

  15. On the Dangers of Rosy Lenses: Reply to Alba, Kasinitz and Waters

    ERIC Educational Resources Information Center

    Haller, William; Portes, Alejandro; Lynch, Scott M.

    2011-01-01

    This article responds to the Alba, Kasinitz and Waters' commentary on the authors' article. The authors state that not all kids are doing "all right," and the substantial number at risk of social and economic stagnation or downward mobility looms as a significant social problem. They contend it is true that right-wing commentators may pick on…

  16. Diversity in seed production characteristics within the USDA-ARS Limnanthes alba germplasm collection

    Technology Transfer Automated Retrieval System (TEKTRAN)

    Meadowfoam (L. alba) seeds are a source of long chain fatty acids which are stable under diverse environmental conditions. The fatty acid composition makes the oil valuable for use in cosmetics, lubricants, rubber additives, and plastics. While a few meadowfoam cultivars have been developed, high se...

  17. Measuring Mars sand flux seasonality from a time series of HiRISE images and calibrating the threshold for sand mobility

    NASA Astrophysics Data System (ADS)

    Ayoub, F.; Avouac, J.; Newman, C. E.; Richardson, M. I.; Lucas, A.; Leprince, S.; Bridges, N. T.

    2013-12-01

    In this study, focused on the Nili Patera dune field on Mars, we measured the temporal variation of the migration rate of sand ripples from the correlation of a time-series of HiRISE images using COSI-Corr. The time-series covers approximately 1.5 Mars year which allows us to observe seasonal migration rate variability as well as taking an early glimpse on yearly variation. A Principal Component Analysis (PCA) was applied to the time-series to quantify more robustly the time evolution of the signal and filter out noise, in particular due to unrecorded satellite jitter. Using the first two components, which account for 82% of the variance, the seasonal variation of the ripple migration rate was estimated. We clearly observe continuously active migration throughout the year with a strong seasonal quasi-sinusoidal variation which peaks at perihelion. Coupling between surface winds and sand transport is a fundamental factor governing geological activity and climate on Mars. Saltation of sand is likely crucial for both erosion of the surface and for the emission of finer (dust) particles into the atmosphere. Analysis of the distinctive seasonal variation of sand flux with an atmospheric model is used to infer an effective threshold for sand motion. This is the first direct estimate of the stress threshold at Mars on spatial scales relevant for dynamical atmospheric modeling of sand transport, surface erosion, and dust lifting.

  18. Small-scale volcanoes on Mars: distribution and types

    NASA Astrophysics Data System (ADS)

    Broz, Petr; Hauber, Ernst

    2015-04-01

    Volcanoes differ in sizes, as does the amount of magma which ascends to a planetary surface. On Earth, the size of volcanoes is anti-correlated with their frequency, i.e. small volcanoes are much more numerous than large ones. The most common terrestrial volcanoes are scoria cones (Mars is a planet which was volcanically active over most (if not all) of its history, a similar distribution of volcano size might be expected. Martian small-scale volcanoes were not intensely studied for a long time due to a lack of high-resolution data enabling their proper identification; however their existence and basic characteristics were predicted on theoretical grounds. Streams of new high-resolution images now enable discovering and studying kilometer-size volcanoes with various shapes in unprecedented detail. Several types of small-scale volcanoes in various regions on Mars were recently described. Scoria cones provide a record of magmatic volatile content and have been identified in Tharsis (Ulysses Colles), on flanks of large volcanoes (e.g., Pavonis Mons), in the caldera of Ulysses Patera, in chaotic terrains or other large depressions (Hydraotes Colles, Coprates Chasma) and in the northern lowlands. Tuff rings and tuff cones, formed as a result of water-magma interaction, seem to be relatively rare on Mars and were only tentatively identified in three locations (Nepenthes/Amenthes region, Arena Colles and inside Lederberg crater), and alternative interpretations (mud volcanoes) seem possible. Other relatively rare volcanoes seem to be lava domes, reported only from two regions (Acracida Planitia and Terra Sirenum). On the other hand, small shields and rootless cones (which are not primary volcanic landforms) represent widely spread phenomena recognized in Tharsis and Elysium. Based on these new observations, the distribution of small volcanoes on Mars seems to be much more widespread than anticipated a decade

  19. Fluvial valleys and Martian palaeoclimates

    NASA Astrophysics Data System (ADS)

    Gulick, Virginia C.; Baker, Victor R.

    1989-10-01

    Theoretical models of early Martian atmospheric evolution describe the maintenance of a dense CO2 atmosphere and a warm, wet climate until the end of the heavy-bombardment phase of impacting. However, the presence of very young, earthlike fluvial valleys on the northern flank of Alba Patera conflicts with this scenario. Whereas the widespread ancient Martian valleys generally have morphologies indicative of sapping erosion by the slow outflow of subsurface water, the local Alba valleys were probably formed by surface-runoff processes. Because subsurface water flow might be maintained by hydrothermal energy inputs and because surface-runoff valleys developed late in Martian history, it is not necessary to invoke drastically different planet-wide climatic conditions to explain valley development on Mars. The Alba fluvial valleys can be explained by hydrothermal activity or outflow-channel discharges that locally modified the atmosphere, including precipitation and local overland flow on low-permeability volcanic ash.

  20. Quick trips to Mars

    NASA Technical Reports Server (NTRS)

    Hornung, R.

    1991-01-01

    The design of a Mars Mission Vehicle that would have to be launched by two very heavy lift launch vehicles is described along with plans for a mission to Mars. The vehicle has three nuclear engine for rocket vehicle application (NERVA) boosters with a fourth in the center that acts as a dual mode system. The fourth generates electrical power while in route, but it also helps lift the vehicle out of earth orbit. A Mars Ascent Vehicle (MAV), a Mars transfer vehicle stage, and a Mars Excursion Vehicle (MEV) are located on the front end of this vehicle. Other aspects of this research including aerobraking, heat shielding, nuclear thermal rocket engines, a mars mission summary, closed Brayton cycle with and without regeneration, liquid hydrogen propellant storage, etc. are addressed.

  1. Mars Solar Power

    NASA Technical Reports Server (NTRS)

    Landis, Geoffrey A.; Kerslake, Thomas W.; Jenkins, Phillip P.; Scheiman, David A.

    2004-01-01

    NASA missions to Mars, both robotic and human, rely on solar arrays for the primary power system. Mars presents a number of challenges for solar power system operation, including a dusty atmosphere which modifies the spectrum and intensity of the incident solar illumination as a function of time of day, degradation of the array performance by dust deposition, and low temperature operation. The environmental challenges to Mars solar array operation will be discussed and test results of solar cell technology operating under Mars conditions will be presented, along with modeling of solar cell performance under Mars conditions. The design implications for advanced solar arrays for future Mars missions is discussed, and an example case, a Martian polar rover, are analyzed.

  2. Mars Surface Habitability Options

    NASA Technical Reports Server (NTRS)

    Howe, A. Scott; Simon, Matthew; Smitherman, David; Howard, Robert; Toups, Larry; Hoffman, Stephen J.

    2015-01-01

    This paper reports on current habitability concepts for an Evolvable Mars Campaign (EMC) prepared by the NASA Human Spaceflight Architecture Team (HAT). For many years NASA has investigated alternative human Mars missions, examining different mission objectives, trajectories, vehicles, and technologies; the combinations of which have been referred to as reference missions or architectures. At the highest levels, decisions regarding the timing and objectives for a human mission to Mars continue to evolve while at the lowest levels, applicable technologies continue to advance. This results in an on-going need for assessments of alternative system designs such as the habitat, a significant element in any human Mars mission scenario, to provide meaningful design sensitivity characterizations to assist decision-makers regarding timing, objectives, and technologies. As a subset of the Evolvable Mars Campaign activities, the habitability team builds upon results from past studies and recommends options for Mars surface habitability compatible with updated technologies.

  3. Cars on Mars

    NASA Technical Reports Server (NTRS)

    Landis, Geoffrey A.

    2002-01-01

    Mars is one of the most fascinating planets in the solar system, featuring an atmosphere, water, and enormous volcanoes and canyons. The Mars Pathfinder, Global Surveyor, and Odyssey missions mark the first wave of the Planet Earth's coming invasion of the red planet, changing our views of the past and future of the planet and the possibilities of life. Scientist and science-fiction writer Geoffrey A. Landis will present experiences on the Pathfinder mission, the challenges of using solar power on the surface of Mars, and present future missions to Mars such as the upcoming Mars Twin Rovers, which will launch two highly-capable vehicles in 2003 to explore the surface of Mars.

  4. Mars elevation distribution

    NASA Technical Reports Server (NTRS)

    Wu, Sherman S. C.; Howington-Kraus, Annie E.; Ablin, Karyn K.

    1991-01-01

    A Digital Terrain Model (DTM) of Mars was derived with both Mercator and Sinusoidal Equal-Area projections from the global topographic map of Mars (scale 1:15 million, contour interval 1 km). Elevations on the map are referred to Mars' topographic datum that is defined by the gravity field at a 6.1-millibar pressure surface with respect to the center of mass of Mars. The DTM has a resolution at the equator of 1/59.226 degrees (exactly 1 km) per pixel. By using the DTM, the volumetric distribution of Mars topography above and below the datum has previously been calculated. Three types of elevation distributions of Mars' topography were calculated from the same DTM: (1) the frequency distribution of elevations at the pixel resolution; (2) average elevations in increments of 6 degrees in both longitude and latitude; and (3) average elevations in 36 separate blocks, each covering 30 degrees of latitude and 60 degrees of longitude.

  5. Arecibo radar imagery of Mars: The major volcanic provinces

    NASA Astrophysics Data System (ADS)

    Harmon, John K.; Nolan, Michael C.; Husmann, Diana I.; Campbell, Bruce A.

    2012-08-01

    We present Earth-based radar images of Mars obtained with the upgraded Arecibo S-band (λ = 12.6 cm) radar during the 2005-2012 oppositions. The imaging was done using the same long-code delay-Doppler technique as for the earlier (pre-upgrade) imaging but at a much higher resolution (˜3 km) and, for some regions, a more favorable sub-Earth latitude. This has enabled us to make a more detailed and complete mapping of depolarized radar reflectivity (a proxy for small-scale surface roughness) over the major volcanic provinces of Tharsis, Elysium, and Amazonis. We find that vast portions of these regions are covered by radar-bright lava flows exhibiting circular polarization ratios close to unity, a characteristic that is uncommon for terrestrial lavas and that is a likely indicator of multiple scattering from extremely blocky or otherwise highly disrupted flow surfaces. All of the major volcanoes have radar-bright features on their shields, although the brightness distribution on Olympus Mons is very patchy and the summit plateau of Pavonis Mons is entirely radar-dark. The older minor shields (paterae and tholi) are largely or entirely radar-dark, which is consistent with mantling by dust or pyroclastic material. Other prominent radar-dark features include: the "fan-shaped deposits", possibly glacial, associated with the three major Tharsis Montes shields; various units of the Medusae Fossae Formation; a region south and west of Biblis Patera where "Stealth" deposits appear to obscure Tharsis flows; and a number of "dark-halo craters" with radar-absorbing ejecta blankets deposited atop surrounding bright flows. Several major bright features in Tharsis are associated with off-shield lava flows; these include the Olympus Mons basal plains, volcanic fields east and south of Pavonis Mons, the Daedalia Planum flows south of Arsia Mons, and a broad expanse of flows extending east from the Tharsis Montes to Echus Chasma. The radar-bright lava plains in Elysium are

  6. Mars at Opposition

    ERIC Educational Resources Information Center

    Riddle, Bob

    2010-01-01

    On January 29, Mars will reach opposition, a point along its orbit around the Sun where Mars will be directly opposite from the Sun in a two-planet and Sun line-up with the Earth in between. At this opposition, the Earth and Mars will be separated by nearly 100 million km. An opposition is similar to a full Moon in that the planet at opposition…

  7. Instrumentation for Mars Environments

    NASA Technical Reports Server (NTRS)

    Landis, Geoffrey A.

    1997-01-01

    The main portion of the project was to support the "MAE" experiment on the Mars Pathfinder mission and to design instrumentation for future space missions to measure dust deposition on Mars and to characterize the properties of the dust. A second task was to analyze applications for photovoltaics in new space environments, and a final task was analysis of advanced applications for solar power, including planetary probes, photovoltaic system operation on Mars, and satellite solar power systems.

  8. Mars: The Viking discoveries

    NASA Technical Reports Server (NTRS)

    French, B. M.

    1977-01-01

    An overview of the Viking Mars probe is presented. The Viking spacecraft is described and a brief history of the earlier observations and exploration of Mars is provided. A number of the Viking photographs of the Martian surface are presented and a discussion of the experiments Viking performed including a confirmation of the general theory of relativity are reported. Martian surface chemistry is discussed and experiments to study the weather on Mars are reported.

  9. Enhancement of Shelf Life of Button Mushroom, Agaricus bisporus (Higher Basidiomycetes) by Fumigant Application of Lippia alba Essential Oil.

    PubMed

    Vishwakarma, Pratima; Pandey, Abhay K; Mishra, Priyanka; Singh, Pooja; Tripathi, N N

    2015-01-01

    Eleven essential oils isolated from higher plant species were assessed against the four isolates of Verticillium fungicola found on fruiting bodies of Agaricus bisporus. Eucalyptus citriodora and Lippia alba oils were more efficacious and completely inhibited the mycelial growth of fungal isolates. L. alba oil was fungistatic and fungicidal at 10- and 20-µL concentrations against all of the isolates, respectively, and was more potent than E. citriodora oil as well as some prevalent synthetic fungicides such as benomyl, ethylene dibromide, and phosphine. Eighty microliters of L. alba oil protected 500 g of fruiting bodies of A. bisporus for up to 7 d from infection of the fungus under in vivo conditions. The findings strengthen the possibility of L. alba oil as a plant-based protectant to enhance the shelf life of A. bisporus fruiting bodies.

  10. Digital cartography of Mars

    NASA Technical Reports Server (NTRS)

    Batson, R. M.

    1987-01-01

    A medium-resolution Digital Image Model (DIM) of Mars is being compiled. A DIM is a mosaic of radiometrically corrected, photometrically modelled spacecraft images displaying accurate reflectance properties at uniform resolution, and geometrically tied to the best available control. The Mars medium-resolution DIM contains approximately 4700 Viking Orbiter image frames that were used to compile the recently completed 1:2,000,000-scale controlled photomosaic series of Mars. This DIM provides a planimetric control base to which all other Mars maps will be registered. A similar control base of topographic elevations (Digital Terrain Model, or DTM) is also being compiled. These products are scheduled for completion in 1989.

  11. Mars - Destination and challenge

    NASA Astrophysics Data System (ADS)

    Aldrich, Arnold D.

    A general evaluation is conducted of the challenges associated with prospective Mars exploration efforts. The technical challenge posed stems from the unforgiving physical environment of space travel, and such peculiarities of Mars as its great orbital eccentricity and 15-year cyclic variation in transfer energy. Additional considerations arise from the 'architecture' of NASA's Space Exploration Initiative, encompassing the determination of a Mars exploration effort's purpose, scope, and schedule. Finally, numerous unresolved issues arise from the definition of detailed scientific experimentation that is to be done for the sake of the greatest long-term benefit to an understanding of Mars, and the rallying of political support behind a major new exploration initiative.

  12. Mars - Destination and challenge

    NASA Technical Reports Server (NTRS)

    Aldrich, Arnold D.

    1992-01-01

    A general evaluation is conducted of the challenges associated with prospective Mars exploration efforts. The technical challenge posed stems from the unforgiving physical environment of space travel, and such peculiarities of Mars as its great orbital eccentricity and 15-year cyclic variation in transfer energy. Additional considerations arise from the 'architecture' of NASA's Space Exploration Initiative, encompassing the determination of a Mars exploration effort's purpose, scope, and schedule. Finally, numerous unresolved issues arise from the definition of detailed scientific experimentation that is to be done for the sake of the greatest long-term benefit to an understanding of Mars, and the rallying of political support behind a major new exploration initiative.

  13. 2001 Mars Odyssey

    NASA Astrophysics Data System (ADS)

    Russell, C. T.

    2004-04-01

    Mars, the most habitable of our sister planets, holds a special place in our imaginations and in our space exploration program. Fully half of NASA's planetary exploration effort is now devoted to Mars. Key questions include: Has Mars ever harbored life? Is there life on Mars now? Will humans be able to survive on the Martian surface? Answers to these questions lie in determining the present location of water on Mars and its likely inventory in the past, and in determining the present radiation environment of Mars. The 2001 Mars Odyssey Mission contributes greatly these answers by detecting near-surface water through measurements of neutron flux, from the detection of carbonates, and the quantification of its radiation environment. This book captures the objectives, the design of the mission and the details of the instruments carried to Mars. It should be of interest to every scientist interested in participating in the on-going exploration of Mars from graduate students to senior scientists as it provides the background information essential to interpret the many exciting results now appearing from the mission. Link: http://www.wkap.nl/prod/b/1-4020-1696-4

  14. Mars Museum Visualization Alliance

    NASA Astrophysics Data System (ADS)

    Sohus, A. M.; Viotti, M. A.; de Jong, E. M.

    2004-11-01

    The Mars Museum Visualization Alliance is a collaborative effort funded by the Mars Public Engagement Office and supported by JPL's Informal Education staff and the Solar System Visualization Project to share the adventure of exploration and make Mars a real place. The effort started in 2002 with a small working group of museum professionals to learn how best to serve museum audiences through informal science educators. By the time the Mars Exploration Rovers landed on Mars in January 2004, over 100 organizations were partners in the Alliance, which has become a focused community of Mars educators. The Alliance provides guaranteed access to images, information, news, and resources for use by the informal science educators with their students, educators, and public audiences. Thousands of people have shared the adventure of exploring Mars and now see it as a real place through the efforts of the Mars Museum Visualization Alliance partners. The Alliance has been lauded for "providing just the right inside track for museums to do what they do best," be that webcasts, live presentations with the latest images and information, high-definition productions, planetarium shows, or hands-on educational activities. The Alliance is extending its mission component with Cassini, Genesis, Deep Impact, and Stardust. The Mars Exploration and Cassini Programs, as well as the Genesis, Deep Impact, and Stardust Projects, are managed for NASA by the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California.

  15. Mars Stratigraphy Mission

    NASA Technical Reports Server (NTRS)

    Budney, C. J.; Miller, S. L.; Cutts, J. A.

    2000-01-01

    The Mars Stratigraphy Mission lands a rover on the surface of Mars which descends down a cliff in Valles Marineris to study the stratigraphy. The rover carries a unique complement of instruments to analyze and age-date materials encountered during descent past 2 km of strata. The science objective for the Mars Stratigraphy Mission is to identify the geologic history of the layered deposits in the Valles Marineris region of Mars. This includes constraining the time interval for formation of these deposits by measuring the ages of various layers and determining the origin of the deposits (volcanic or sedimentary) by measuring their composition and imaging their morphology.

  16. A Mars base

    NASA Technical Reports Server (NTRS)

    Soule, Veronique

    1989-01-01

    This study was initiated to provide an approach to the development of a permanently manned Mars base. The objectives for a permanently manned Mars base are numerous. Primarily, human presence on Mars will allow utilization of new resources for the improvement of the quality of life on Earth, allowing for new discoveries in technologies, the solar system, and human physiology. Such a mission would also encourage interaction between different countries, increasing international cooperation and leading to a stronger unification of mankind. Surface studies of Mars, scientific experiments in the multiple fields, the research for new minerals, and natural resource production are more immediate goals of the Mars mission. Finally, in the future, colonization of Mars will ensure man's perpetual presence in the universe. Specific objectives of this study were: (1) to design a Mars habitat that minimizes the mass delivered to the Mars surface, provides long-stay capability for the base crew, and accommodates future expansion and modification; (2) to develop a scenario of the construction of a permanently manned Mars base; and (3) to incorporate new and envisioned technologies.

  17. Exobiology and Future Mars Missions

    NASA Technical Reports Server (NTRS)

    Mckay, Christopher P. (Editor); Davis, Wanda, L. (Editor)

    1989-01-01

    Scientific questions associated with exobiology on Mars were considered and how these questions should be addressed on future Mars missions was determined. The mission that provided a focus for discussions was the Mars Rover/Sample Return Mission.

  18. Radar, visual and thermal characteristics of Mars: Rough planar surfaces

    USGS Publications Warehouse

    Schaber, G.G.

    1980-01-01

    High-resolution Viking Orbiter images (10 to 15 m/pixel) contain significant information on Martian surface roughness at 25- to 100-m lateral scales, whereas Earth-based radar observations of Mars are sensitive to roughness at lateral scales of 1 to 30 m, or more. High-rms slopes predicted for the Tharsis-Memnonia-Amazonis volcanic plains from extremely weak radar returns (low peak radar cross section) are qualitatively confirmed by the Viking image data. Large-scale, curvilinear (but parallel) ridges on lava flows in the Memnonia Fossae region are interpreted as innate flow morphology caused by compressional foldover of moving lava sheets of possible rhyolite-dacite composition. The presence or absence of a recent mantle of fine-grained eolian material on the volcanic surfaces studied was determined by the visibility of fresh impact craters with diameters less than 50 m. Lava flows south and west of Arsia Mons, and within the large region of low thermal inertia centered on Tharsis Montes (H. H. Kieffer et al., 1977, J. Geophys. Res.82, 4249-4291), were found to possess such a recent mantle. At predawn residual temperatures ??? -10K (south boundary of this low-temperature region), lava flows are shown to have relatively old eolian mantles. Lava flows with surfaces modified by eolian erosion and deposition occur west-northwest of Apollinaris Patera at the border of the cratered equatorial uplands and southern Elysium Planitia. Nearby yardangs, for which radar observations indicate very high-rms slopes, are similar to terrestrial features of similar origin. ?? 1980.

  19. Evidence for explosive volcanism in Arabia Terra, Mars

    NASA Astrophysics Data System (ADS)

    Michalski, Joseph; Bleacher, Jacob

    2014-05-01

    Several irregularly shaped craters located within Arabia Terra, Mars, represent a new type of volcanic construct and together constitute a previously unrecognized Martian igneous province. Similar to terrestrial supervolcanoes, these low-relief paterae exhibit a range of geomorphic features related to structural collapse, effusive volcanism and explosive eruptions. They were likely active in the Late Noachian or Early Hesperian and would have affected the climate, atmospheric composition, and regional surface geology at that time. Lavas extruded from these calderas contributed to the formation of enigmatic highland ridged plains in Arabia Terra, but these volcanoes do not exhibit shield-like topographic profiles related to the sustained, localized effusive eruption of basaltic lava. We suggest that the lack of a single edifice, the large volume of collapse within an associated with the calderas, and the association of the calderas with vast deposits friable clastic deposits all indicate that these volcanoes were dominated by explosive activity. Layered, friable deposits found throughout Arabia Terra have enigmatic origins, though these materials have been suggested to represent volcanic ash. Attempts to link the locations of various friable deposits in equatorial regions to known volcanic sources have demonstrated that this hypothesis is plausible, but a link between friable deposits and known volcanic sources in this particular region (Arabia Terra) has yet to emerge. We suggest that some of the layered, friable materials were sourced from calderas in Arabia Terra. Outgassed sulphur and water from these calderas would have contributed to the alteration of layered clastic materials in Arabia Terra, and perhaps throughout the equatorial region.

  20. Inhibitory effect of linalool-rich essential oil from Lippia alba on the peptidase and keratinase activities of dermatophytes.

    PubMed

    Costa, Danielle Cristina Machado; Vermelho, Alane Beatriz; Almeida, Catia Amancio; de Souza Dias, Edilma Paraguai; Cedrola, Sabrina Martins Lage; Arrigoni-Blank, Maria de Fátima; Blank, Arie Fitzgerald; Alviano, Celuta Sales; Alviano, Daniela Sales

    2014-02-01

    Abstract Lippia alba (Miller) N.E. Brown is an aromatic plant known locally as "Erva-cidreira-do-campo" that has great importance in Brazilian folk medicine. The aim of our study was to evaluate the antidermatophytic potential of linalool-rich essential oil (EO) from L. alba and analyze the ability of this EO to inhibit peptidase and keratinase activities, which are important virulence factors in dermatophytes. The minimum inhibitory concentrations (MICs) of L. alba EO were 39, 156 and 312 µg/mL against Trichophyton rubrum, Epidermophyton floccosum and Microsporum gypseum, respectively. To evaluate the influence of L. alba EO on the proteolytic and keratinolytic activities of these dermatophytes, specific inhibitory assays were performed. The results indicated that linalool-rich EO from L. alba inhibited the activity of proteases and keratinases secreted from dermatophytes, and this inhibition could be a possible mechanism of action against dermatophytes. Due to the effective antidermatophytic activity of L. alba EO, further experiments should be performed to explore the potential of this linalool-rich EO as an alternative antifungal therapy.

  1. Review of NASA's Planned Mars Program

    NASA Technical Reports Server (NTRS)

    1996-01-01

    Contents include the following: Executive Summary; Introduction; Scientific Goals for the Exploration of Mars; Overview of Mars Surveyor and Others Mars Missions; Key Issues for NASA's Mars Exploration Program; and Assessment of the Scientific Potential of NASA's Mars Exploration Program.

  2. Rat on Mars

    NASA Technical Reports Server (NTRS)

    2004-01-01

    This image taken on Mars by the panoramic camera on the Mars Exploration Rover Opportunity shows the rover's rock abrasion tool, also known as 'rat' (circular device in center), located on its instrument deployment device, or 'arm.' The image was acquired on the ninth martian day or sol of the rover's mission.

  3. Microscope on Mars

    NASA Technical Reports Server (NTRS)

    2004-01-01

    This image taken at Meridiani Planum, Mars by the panoramic camera on the Mars Exploration Rover Opportunity shows the rover's microscopic imager (circular device in center), located on its instrument deployment device, or 'arm.' The image was acquired on the ninth martian day or sol of the rover's mission.

  4. Is Mars Red Hot?

    NASA Video Gallery

    What would it feel like if you could stand on Mars – toasty warm, or downright chilly? Find out more about the temperature on Mars in this 60-second video from NASA’s Jet Propulsion Laboratory.

  5. The Mars Millennium Project.

    ERIC Educational Resources Information Center

    National Aeronautics and Space Administration, Washington, DC.

    The countdown to a new century provides a unique opportunity to engage America's youth in charting a course for the future. The Mars Millennium Project challenges students across the nation to design a community yet to be imagined for the planet Mars. This interdisciplinary learning project aims to encourage K-12 students in classrooms and youth…

  6. Mars Exploratory Vehicles.

    ERIC Educational Resources Information Center

    Canizo, Thea L.; And Others

    1997-01-01

    Presents an activity in which students learn about the characteristics of the planet Mars. Challenges students to design and build a model of a robotic vehicle that can travel on the surface of Mars and accomplish an assigned task that will provide information useful for future manned trips to the planet. Outlines mission task cards and progress…

  7. The channels of Mars

    NASA Technical Reports Server (NTRS)

    Baker, Victor R.

    1988-01-01

    The geomorphology of Mars is discussed, focusing on the Martian channels. The great flood channels of Mars, the processes of channel erosion, and dendritic channel networks, are examined. The topography of the Channeled Scabland region of the northwestern U.S. is described and compared to the Martian channels. The importance of water in the evolution of the channel systems is considered.

  8. Mars transfer vehicle studies

    NASA Technical Reports Server (NTRS)

    Woodcock, Gordon

    1993-01-01

    Earth-to-Mars distances vary from 60 to 400 million kilometers over a 14-year cycle. This complicates Mars mission design as a function of calendar time. Stay times at Mars are also strongly driven by opportunities for a return flight path which are within the limits of delta-V associated with practical space vehicles. The biggest difference between Mars and lunar transfer missions is mission time, which grows from a few days for the moon, to as much as a few hundred days for Mars missions. As a result, modules for similarly sized crews must be much larger for Mars missions that for transfer to lunar orbit. Technology challenges for one Mars mission scenario analyzed by Boeing include aerobrakes, propulsion, and life support systems. Mission performance is very sensitive to aerobrake weight fraction and, as a result, there is an incentive to use high performance materials such as advanced composites and thermal protection systems. Lander aerobrake would be used twice (for both planetary capture and descent to the Mars surface), and it would need to survive temperatures up to 3500 degrees.

  9. Mars' grand finale

    SciTech Connect

    Parker, D.C.; Beish, J.D.; Hernandez, C.E.

    1989-04-01

    Results are presented from observations of the 1988 Mars apparition. Consideration is given to observations of the Martian south polar cap, meteorological activity on the planet, and changes in the surface features of Mars during the apparition. Also, the Martian dust storms observed in November 1988 are described.

  10. Mars ice caps.

    PubMed

    Leovy, C

    1966-12-02

    Minimum atmospheric temperatures required to prevent CO(2) condensatio in the Mars polar caps are higher than those obtained in a computer experiment to simulate the general circulation of the Mars atmosphere. This observation supports the view that the polar caps are predominantly solid CO(2). However, thin clouds of H(2)0 ice could substantially reduce the surface condensation rate.

  11. Viking Mars encounter

    NASA Technical Reports Server (NTRS)

    1976-01-01

    Various phases of planetary operations related to the Viking mission to Mars are described. Topics discussed include: approach phase, Mars orbit insertion, prelanding orbital activities, separation, descent and landing, surface operations, surface sampling and operations starting, orbiter science and radio science, Viking 2, Deep Space Network and data handling.

  12. Plasma engineering for MARS

    SciTech Connect

    Carlson, G.A.; Baldwin, D.E.; Barr, W.L.

    1983-03-24

    The two-year Mirror Advanced Reactor Study (MARS) has resulted in the conceptual design of a commercial, electricity-producing fusion reactor based on tandem mirror confinement. The physics basis for the MARS reactor was developed through work in two highly coupled areas of plasma engineering: magnetics and plasma performance.

  13. Geologic Evolution of Dao Vallis, Mars

    NASA Astrophysics Data System (ADS)

    Crown, D. A.; Bleamaster, L. F.; Mest, S. C.

    2003-12-01

    Three major outflow channel systems (Dao, Harmakhis, and Reull Vallis) extend through the cratered highlands and sedimentary plains of the eastern Hellas region of Mars. These valles represent a stage in regional geologic history intermediate to formation of channels and valleys within highland terrains in the Late Noachian and Early Hesperian Epochs and debris aprons and gullies in the Amazonian Period. Dao Vallis, along with its tributary Niger Vallis, extends for ~1200 km from the eastern margin of Hadriaca Patera into Hellas Planitia, where a depositional lobe is observed on the basin floor. The Dao Vallis system (~6-50 km wide) is characterized by two steep-walled source depressions, regions of subsided plains, and prominent central canyons whose walls display gullies with associated depositional aprons covering parts of canyon floors. The present study is designed to utilize MOC images, MOLA topographic data, and THEMIS daytime and nighttime images to evaluate and refine the geologic evolution of Dao Vallis as defined in earlier Viking-based studies. Dao Vallis has previously been interpreted to have formed by collapse of volcanic and sedimentary plains, potentially triggered by volcano-ice interactions in the Martian subsurface. Small channels and lineations parallel to canyon walls provide evidence for surface flow of fluids. Evidence for subsurface flow is present in zones of subsided plains that separate the central canyons of Dao and Niger Valles from their source depressions. Later stages of the geologic history were dominated by mass-wasting from canyon walls, which may have significantly increased canyon width in places. Comparison of MOC, THEMIS, and Viking images suggests a consistency of geologic processes across a range of spatial scales, as evidence for collapse, mass-wasting, and fluvial erosion and deposition is observed in all datasets. The higher spatial resolution of MOC and THEMIS permits a more detailed understanding of Dao Vallis

  14. Pharmacognostical Standardization of Upodika- Basella alba L.: An Important Ayurvedic Antidiabetic Plant

    PubMed Central

    Shantha, T R; Patchaimal, P; Reddy, M Prathapa; Kumar, R Kishore; Tewari, Devesh; Bharti, Vandana; Venkateshwarlu, G; Mangal, A K; Padhi, M M; Dhiman, K S

    2016-01-01

    Objective: To establish the pharmacognostic standards for the correct identification and standardization of an important Antidiabetic plant described in Ayurveda. Materials and Methods: Standardization was carried out on the leaf and stem of Basella alba L. with the help of the macro-morphological, microscopic, physicochemical and qualitative phytochemical studies. Results: Several specific characters were identified viz. clustered calcium oxalate crystals in the cortex region, absence of trichomes, succulent, thick, mucilaginous, fibrous stem. Rubiaceous type of stomata on both sides of the leaf. Quantitative microscopy along with physicochemical and qualitative phytochemical analysis were also established. Conclusion: The pharmacognostic standards could serve as the reference for the proper identification of the Basella alba L. which is an important anti-diabetic plant described in Ayurveda. PMID:28182032

  15. The ALBA spectroscopic LEEM-PEEM experimental station: layout and performance

    PubMed Central

    Aballe, Lucia; Foerster, Michael; Pellegrin, Eric; Nicolas, Josep; Ferrer, Salvador

    2015-01-01

    The spectroscopic LEEM-PEEM experimental station at the CIRCE helical undulator beamline, which started user operation at the ALBA Synchrotron Light Facility in 2012, is presented. This station, based on an Elmitec LEEM III microscope with electron imaging energy analyzer, permits surfaces to be imaged with chemical, structural and magnetic sensitivity down to a lateral spatial resolution better than 20 nm with X-ray excited photoelectrons and 10 nm in LEEM and UV-PEEM modes. Rotation around the surface normal and application of electric and (weak) magnetic fields are possible in the microscope chamber. In situ surface preparation capabilities include ion sputtering, high-temperature flashing, exposure to gases, and metal evaporation with quick evaporator exchange. Results from experiments in a variety of fields and imaging modes will be presented in order to illustrate the ALBA XPEEM capabilities. PMID:25931092

  16. Therapeutic activity of crude ethanolic extract of Artemisia herba alba against Trypanosoma evansi in rabbits

    NASA Astrophysics Data System (ADS)

    Awad, Fathy M.; Hasan, Zainal Abidin Abu; Osman, Abdinasir Yusuf; Ibrahim, Nazlina

    2013-11-01

    The present work was conducted to evaluate the antitrypanosomal efficacy of crude ethanolic extract (CEE) of the aerial parts of Artemisia herba alba against Trypanosoma evansi infection in an animal model. The results indicated low levels of parasitaemia in rabbits administered with crude ethanolic extract (CEE) compared to those from the negative control group. Similarly, there was also haematologically significant difference (p<0.05) where low mean levels of packed cell volume (PCV) was observed in Groups 1-4 respectively. In contrast, there was no statistically significant difference in almost all investigated parameters between positive control and treatment groups of animals. In conclusion, both CEE of A. herba-alba and Berenil® showed relatively a parasitaemia and normal haematological values in infected rabbits, thereby confirming their antiparasitic properties.

  17. Antibacterial activity of Phyllantus emblica, Coriandrum sativum, Culinaris medic, Lawsonia alba and Cucumis sativus.

    PubMed

    Khan, Dawood Ali; Hassan, Fouzia; Ullah, Hanif; Karim, Sabiha; Baseer, Abdul; Abid, Mobasher Ali; Ubaidi, Muhammad; Khan, Shujaat Ali; Murtaza, Ghulam

    2013-01-01

    Present study deals with the demonstration of the antibacterial activity of very common medicinal plants of Pakistani origin i.e., Phyllantus emblica, Coriandrum sativum, Culinaris medic, Lawsonia alba and Cucumis sativus. The extracts were prepared in crude form by the use of hydro-alcoholic solution and were screened for antibacterial activity against various bacterial species by disk diffusion method. Assay was performed using clinical isolates of B. cereus, S. aureus, P. aeruginosa and E. coli. Crude extract of Phyllantus emblica fruit exhibited strong activity against standard cultures of all studied bacteria. Lawsonia alba showed good activity against standard cultures of all the used microorganisms. Coriandrum sativum was effective only against Bacillus cereus, while Cucumis sativus and Culinaris medic showed poor activity against Pseudomonas aeruginosa only. Hence, Phyllantus emblica exhibited strong antibacterial activity against a wide range of bacteria it means that Phyllantus emblica extract contains some compounds which have broad spectrum of bactericidal activity.

  18. New Mars vehicle concepts

    NASA Astrophysics Data System (ADS)

    Sherwood, Brent

    1993-02-01

    The paper briefly reviews the evolution of the Mars vehicle design concepts from 1952 to 1990, and the currently understood requirements, constraints, and options for manned Mars missions in the early decades of the 21st century. The most up-to-date integrated Mars vehicle concepts for crew-carrying transfer and excursion vehicles are presented together with the Mars descent-ascent mission phases. Particular attention is given to a reusable transfer ship, which is a modular vehicle launched to earth orbit on six 185 t-class boosters and assembled there robotically; it uses dual nuclear-thermal rocket engines and liquid hydrogen propellant. The lander concept is capable of supporting many kinds of surface missions anywhere on Mars.

  19. Mars Observer instrument complement

    NASA Astrophysics Data System (ADS)

    Komro, Fred G.; Hujber, Frank N.

    1991-10-01

    The mechanical and electrical characteristics and the functional designs of the eight scientific instruments of the Mars Observer's instrument complex are described, and their respective principal investigators and sponsoring institutions are listed. These instruments include a gamma-ray spectrometer, a magnetometer/electron reflectometer, the Mars balloon relay, the Mars Observer camera, the Mars Observer laser altimeter, a pressure modulator infrared radiometer, a thermal emission spectrometer, and an ultrastable oscillator. With these instruments, the Mars Observer will be able to determine the elemental and mineralogical character of Martial surface material; to define globally the topography and the gravitational field; to establish the nature of the magnetic field; to determine the spatial and temporal distribution abundances, sources, and sinks of volatile material and dust over a seasonal cycle; and to explore the structure and circulation of Martian atmosphere.

  20. Mars Human Exploration Objectives

    NASA Technical Reports Server (NTRS)

    Briggs, Geoff

    1998-01-01

    This paper reviews the objectives and other considerations of Human exploration of Mars. The objectives of human exploration of Mars are: (1) to learn how Mars is similar to, and different from, Earth; (2) to explore possible life, past and present; (3) to discover what Mars is like now from the perspective of Geoscience and geologic history; and (4) how did Mars form and how did its formation differ from Earth. Considerations of human Martian exploration involve: (1) having a capable base laboratory; (2) having long range transportation; (3) having operational autonomy of the crew, and the requirement of the crew to possess a range of new cognitive processes along with easy communications with terrestrial colleagues; and finally (4) creating the human habitat along with human factors which involve more than just survivability.

  1. Isoprene and terpenoid emissions from Abies alba: Identification and emission rates under ambient conditions

    NASA Astrophysics Data System (ADS)

    Pokorska, Olga; Dewulf, Jo; Amelynck, Crist; Schoon, Niels; Šimpraga, Maja; Steppe, Kathy; Van Langenhove, Herman

    2012-11-01

    In this study, biogenic volatile organic compound (BVOC) emissions from Abies alba were studied under ambient conditions in Flanders (Belgium). Emission patterns and rates were investigated from April till November 2010 by using the dynamic branch enclosure technique. The present work revealed that A. alba is an isoprene emitter, with isoprene accounting for 86-93% of total BVOC emissions, except during budburst (67%) in May. The emission spectrum of A. alba consisted of 27 compounds. Next to isoprene, the main emitted compounds were α-pinene, β-pinene, camphene and limonene. BVOC emissions showed a peak in June after development of the young needles, followed by a constant emission during summer months and September and a decrease in October. In all the samples isoprene was the most abundant compound with standardized emission rates between 27 μg g(dw)-1 h-1 in June and 4.6 μg g(dw)-1 h-1 in October, while the total standardized terpenoid emission rates ranged from 2.85 μg g(dw)-1 h-1 in June to 0.26 μg g(dw)-1 h-1 in October. The obtained average β coefficients according to the temperature dependent algorithm of Guenther et al. (1993) during April-June, July, August and September-October were as follows: for terpenoids 0.12 ± 0.03, 0.11 ± 0.05, 0.12 ± 0.04, 0.24 ± 0.01 K-1 and sesquiterpenes (SQTs) 0.09 ± 0.02, 0.11 ± 0.01, 0.10 ± 0.05, 0 K-1, respectively. Overall, isoprene detected in this study was never quantified in previous studies on A. alba and this finding could have a significant impact on the regional BVOCs budget. Therefore, the result of this study is very important for modeling and local air quality.

  2. New Improvements in Magnetic Measurements Laboratory of the ALBA Synchrotron Facility

    NASA Astrophysics Data System (ADS)

    Campmany, Josep; Marcos, Jordi; Massana, Valentí

    ALBA synchrotron facility has a complete insertion devices (ID) laboratory to characterize and produce magnetic devices needed to satisfy the requirements of ALBA's user community. The laboratory is equipped with a Hall-probe bench working in on-the-fly measurement mode allowing the measurement of field maps of big magnetic structures with high accuracy, both in magnetic field magnitude and position. The whole control system of this bench is based on TANGO. The Hall probe calibration range extends between sub-Gauss to 2 Tesla with an accuracy of 100 ppm. Apart from the Hall probe bench, the ID laboratory has a flipping coil bench dedicated to measuring field integrals and a Helmholtz coil bench specially designed to characterize permanent magnet blocks. Also, a fixed stretched wire bench is used to measure field integrals of magnet sets. This device is specifically dedicated to ID construction. Finally, the laboratory is equipped with a rotating coil bench, specially designed for measuring multipolar devices used in accelerators, such as quadrupoles, sextupoles, etc. Recent improvements of the magnetic measurements laboratory of ALBA synchrotron include the design and manufacturing of very thin 3D Hall probe heads, the design and manufacturing of coil sensors for the Rotating coil bench based on multilayered PCB, and the improvement of calibration methodology in order to improve the accuracy of the measurements. ALBA magnetic measurements laboratory is open for external contracts, and has been widely used by national and international institutes such as CERN, ESRF or CIEMAT, as well as magnet manufacturing companies, such as ANTEC, TESLA and I3 M. In this paper, we will present the main features of the measurement benches as well as improvements made so far.

  3. Properties of the Medussae Fossae Formation and its relation to the volcanic history of Mars

    NASA Astrophysics Data System (ADS)

    Ivanov, Anton B.; Cantini, Federico

    2016-10-01

    Medussae Fossae (MFF) is a well known formation, stretching west of Tharsis volanoes. It is characterized as a relatively young Amazonian units (Amm, Amu), due to widespread signs of erosion. Earth based imaging radar observations at 3.5 cm [1] and 12 cm [2] have discovered a dark radar feature (Stealth), which roughly correlates with the MFF outline.Recent investigations [3], suggested that the unit emplacement is in fact during Hesperian period, but it is composed of material that can be easily eroded. It is not clear when the erosion happened and if it is a continuing process. Hypotheses on MFF formation range from volcanic material emplacement (ash flow tuffs or pyroclastic materials) to an ice-rich dusty mantle, deposited during high obliquity.In this work, we will present the latest observations of the East Medussae Fossae formation by the long wavelength MARSIS radar, continuing the work reported in [4], as well as complementing data surveyed by SHARAD data in [5]. The MARSIS radar has detected strong subsurface interfaces in the areas of Gordi and Eumenides Dorsae at depths up to 1.5km. We will present our analysis of the data, inferring the dielectric properties of the material to constrain properties of the material constituting the Medusae Fossae formation. We will also demonstrate an efficient user interface to work with MARSIS data inside a Geographical Information System (GIS).The research leading to these results has received funding from the European Unions Seventh Framework Programme (FP7/2007-2013) under iMars grant agreement 607379.[1] D. Muhleman, et al., "Radar images of mars," Science, vol. 253, no. 5027, 1991.[2] J. K. Harmon, et al., "Arecibo radar imagery of Mars: The major volcanic provinces," Icarus, vol. 220, aug 2012.[3] L. Kerber, et al., "The dispersal of pyroclasts from Apollinaris Patera, Mars: Implications for the origin of the Medusae Fossae Formation," Icarus, vol. 216, nov 2011.[4] T. R. Watters, et al., "Radar Sounding of the

  4. Improved Chemotherapeutic Activity by Morus alba Fruits through Immune Response of Toll-Like Receptor 4

    PubMed Central

    Chang, Bo Yoon; Kim, Seon Beom; Lee, Mi Kyeong; Park, Hyun; Kim, Sung Yeon

    2015-01-01

    Morus alba L. fruits have long been used in traditional medicine by many cultures. Their medicinal attributes include cardiovascular, hepatoprotective, neuroprotective and immunomodulatory actions. However, their mechanism of macrophage activation and anti-cancer effects remain unclear. The present study investigated the molecular mechanisms of immune stimulation and improved chemotherapeutic effect of M. alba L. fruit extract (MFE). MFE stimulated the production of cytokines, nitric oxide (NO) and tumor necrosis factor-α (TNF-α) and tumoricidal properties of macrophages. MFE activated macrophages through the mitogen-activated protein kinase (MAPKinase) and nuclear factor-κB (NF-κB) signaling pathways downstream from toll-like receptor (TLR) 4. MFE was shown to exhibit cytotoxicity of CT26 cells via the activated macrophages, even though MFE did not directly affect CT26 cells. In a xenograft mouse model, MFE significantly enhanced anti-cancer activity combined with 5-fluorouracil and markedly promoted splenocyte proliferation, natural killer (NK) cell activity, cytotoxic T lymphocyte (CTL) activity and IFN-γ production. Immunoglobulin G (IgG) antibody levels were significantly increased. These results indicate the indirect anti-cancer activity of MFE through improved immune response mediated by TLR4 signaling. M. alba L. fruit extract might be a potential anti-tumor immunomodulatory candidate chemotherapy agent. PMID:26473845

  5. Release and dispersal of basidiospores from Amanita muscaria var. alba and their infiltration into a residence.

    PubMed

    Li, De-Wei

    2005-11-01

    Release and dispersal of basidiospores of Amanita muscaria var. alba and their potential to infiltrate a nearby residence were investigated. Basidiospore release mainly occurred in the first three days following the expansion of the caps. The concentrations of released basidiospores near basidiomata were 77 137, 75 062, and 41 738 spores m(-3) in the first three days, respectively, with the highest concentration at 281 738 spores m(-3) air. After three days, the concentration dropped by 95%. At the second location, airborne basidiospore concentrations dropped 96-99% after three days with the concentrations of 940, 575, and 1359 spores m(-3) in the first three days, respectively. The diurnal pattern showed a relatively extended night peak. Relative humidity and dew were positively correlated with basidiospore release and short distance dispersal. Rain and rain rate were positively correlated with basidiospore release, but not correlated with short distance dispersal. The basidiospore release period of Amanita muscaria var. alba was short, but within such a period it released a large amount of basidiospores. However, only less than 5% of basidiospores released were dispersed to the second location 5.2 m away and 2.7 m above the basidiomata. Only < 0.1% of basidiospores dispersed from the basidiomata were found inside a nearby residence. Amanita muscaria var. alba showed a low potential of infiltrating the residence.

  6. HPLC profiles and biomarker contents of Australian-grown Salvia miltiorrhiza f. alba roots.

    PubMed

    Li, Chun Guang; Sheng, Shu Jun; Pang, Edwin C K; May, Brian; Xue, Charlie Chang Li

    2009-07-01

    Salvia miltiorrhiza f. alba (Baihua Danshen) is a Chinese medicinal herb commonly used for treating cardiovascular disease. It has been grown in Australia, although the quality of its main medicinal part (dried root) has not been assessed. In this study, we investigated HPLC profiles and biomarker contents of Australian-grown S. miltiorrhiza f. alba roots. Patterns of HPLC profiles were established in MeOH, and aqueous extracts in terms of number of common characteristic peaks and their relative retention times. The contents of three tanshinone biomarkers (cryptotanshinone (3), tanshinone I (1), and tanshinone IIA (2)) were significantly higher (p<0.05) in the roots of one-year-old plants than those of two-year-old plants. In contrast, salvianolic acid B (4) content was significantly higher in the roots of two-year-old plants than in those of one-year-old plants. The findings suggest that the biomarker contents in Australian-grown S. miltiorrhiza f. alba roots vary with the growth periods of the plants, which may be important in determining the optimal harvest time for the plant roots with targeted levels of tanshinones and salvianolic acid B (4).

  7. Karyotype analysis, DNA content and molecular screening in Lippia alba (Verbenaceae).

    PubMed

    Pierre, Patrícia M O; Sousa, Saulo M; Davide, Lisete C; Machado, Marco A; Viccini, Lyderson F

    2011-09-01

    Cytogenetic analyses, of pollen viability, nuclear DNA content and RAPD markers were employed to study three chemotypes of Lippia alba (Mill.) (Verbenaceae) in order to understand the genetic variation among them. Different ploidy levels and mixoploid individuals were observed. This work comprises the first report of different chromosome numbers (cytotypes) in L. alba. The chromosome numbers of La2-carvone and La3-linalool chemotypes suggested that they are polyploids. Flow cytometric analysis showed an increase of nuclear DNA content that was not directly proportional to ploidy level variation. A cluster analysis based on RAPD markers revealed that La3-linalool shares genetic markers with La1-citral and La2-carvone. The analysis showed that the majority of genetic variation of La3-linalool could be a consequence of ixoploidy. ur data indicates that sexual reproduction aong those three chemotypes is unlikely and suggests the beginning of reproductive isolation. The results demonstrated that chromosome analysis, nuclear DNA content estimation and RAPD markers constitute excellent tools for detecting genetic variation among L. alba chemotypes.

  8. Composition, anti-quorum sensing and antimicrobial activity of essential oils from Lippia alba

    PubMed Central

    Olivero-Verbel, Jesus; Barreto-Maya, Ana; Bertel-Sevilla, Angela; Stashenko, Elena E.

    2014-01-01

    Many Gram-negative pathogens have the ability to produce N-acylhomoserine lactones (AHLs) as signal molecules for quorum sensing (QS). This cell-cell communication system allows them to coordinate gene expression and regulate virulence. Strategies to inhibit QS are promising for the control of infectious diseases or antibiotic resistant bacterial pathogens. The aim of the present study was to evaluate the anti-quorum sensing (anti-QS) and antibacterial potential of five essential oils isolated from Lippia alba on the Tn-5 mutant of Chromobacterium violaceum CV026, and on the growth of the gram-positive bacteria S. aureus ATCC 25923. The anti-QS activity was detected through the inhibition of the QS-controlled violacein pigment production by the sensor bacteria. Results showed that two essential oils from L. alba, one containing the greatest geranial:neral and the other the highest limonene:carvone concentrations, were the most effective QS inhibitors. Both oils also had small effects on cell growth. Moreover, the geranial/neral chemotype oil also produced the maximum zone of growth inhibition against S. aureus ATCC 25923. These data suggest essential oils from L. alba have promising properties as QS modulators, and present antibacterial activity on S. aureus. PMID:25477905

  9. Composition, anti-quorum sensing and antimicrobial activity of essential oils from Lippia alba.

    PubMed

    Olivero-Verbel, Jesus; Barreto-Maya, Ana; Bertel-Sevilla, Angela; Stashenko, Elena E

    2014-01-01

    Many Gram-negative pathogens have the ability to produce N-acylhomoserine lactones (AHLs) as signal molecules for quorum sensing (QS). This cell-cell communication system allows them to coordinate gene expression and regulate virulence. Strategies to inhibit QS are promising for the control of infectious diseases or antibiotic resistant bacterial pathogens. The aim of the present study was to evaluate the anti-quorum sensing (anti-QS) and antibacterial potential of five essential oils isolated from Lippia alba on the Tn-5 mutant of Chromobacterium violaceum CV026, and on the growth of the gram-positive bacteria S. aureus ATCC 25923. The anti-QS activity was detected through the inhibition of the QS-controlled violacein pigment production by the sensor bacteria. Results showed that two essential oils from L. alba, one containing the greatest geranial:neral and the other the highest limonene:carvone concentrations, were the most effective QS inhibitors. Both oils also had small effects on cell growth. Moreover, the geranial/neral chemotype oil also produced the maximum zone of growth inhibition against S. aureus ATCC 25923. These data suggest essential oils from L. alba have promising properties as QS modulators, and present antibacterial activity on S. aureus.

  10. Anti-dopaminergic effect of the methanolic extract of Morus alba L. leaves

    PubMed Central

    Yadav, Adhikrao V.; Nade, Vandana S.

    2008-01-01

    Objective: To evaluate the effect of methanolic extract of Morus alba L. leaves on dopaminergic function. Materials and Methods: The effect of the methanolic extract of Morus alba L. leaves was evaluated on haloperidol and metoclopramide induced catalepsy, foot shock-induced aggression, amphetamine-induced stereotyped behavior and phenobarbitone induced sleeping in mice. In each of these tests, the extract was administered in doses of 50, 100 and 200 mg/kg, i.p., 30 min before performing the test in mice. Further, the inhibitory effect of the extract on dopamine was studied using isolated rat vas deferens. Results: The extract produced significant dose dependent potentiation of haloperidol (1 mg/kg, i.p.) and metoclopramide (20 mg/kg, i.p.) induced catalepsy in mice. The extract significantly reduced number of fights and increased latency to fights in foot shock-induced aggression; it also decreased amphetamine (1 mg/kg, i.p.) induced stereotyped behavior in a dose dependent manner. The sleeping time induced by phenobarbitone (50 mg/kg, i.p.) too was prolonged. The extract inhibited contractions produced by dopamine on isolated rat vas deferens. Conclusion: The results suggest that the methanolic extract of Morus alba L. possesses antidopaminergic activity. Further neurochemical investigation can explore the mechanism of action of the plant drug with respect to antidopaminergic functions and help to establish the plant as an antipsychotic agent. PMID:20040961

  11. Odisolane, a Novel Oxolane Derivative, and Antiangiogenic Constituents from the Fruits of Mulberry (Morus alba L.).

    PubMed

    Lee, Seoung Rak; Park, Jun Yeon; Yu, Jae Sik; Lee, Sung Ok; Ryu, Ja-Young; Choi, Sang-Zin; Kang, Ki Sung; Yamabe, Noriko; Kim, Ki Hyun

    2016-05-18

    Mulberry, the fruit of Morus alba L., is known as an edible fruit and commonly used in Chinese medicines as a warming agent and as a sedative, tonic, laxative, odontalgic, expectorant, anthelmintic, and emetic. Systemic investigation of the chemical constituents of M. alba fruits led to the identification of a novel oxolane derivative, (R*)-2-((2S*,3R*)-tetrahydro-2-hydroxy-2-methylfuran-3-yl)propanoic acid (1), namely, odisolane, along with five known heterocyclic compounds (2-6). The structure of the new compound was elucidated on the basis of HR-MS, 1D and 2D NMR ((1)H-(1)H COSY, HSQC, HMBC, and NOESY) data analysis. Compound 1 has a novel skeleton that consists of 8 carbon units with an oxolane ring, which until now has never been identified in natural products. The isolated compounds were subjected to several activity tests to verify their biological function. Among them, compounds 1, 3, and 5 significantly inhibited cord formation in HUVECs. The action mechanism of compound 3, which had the strongest antiangiogenic activity, was mediated by decreasing VEGF, p-Akt, and p-ERK protein expression. These results suggest that compounds isolated from M. alba fruits might be beneficial in antiangiogenesis therapy for cancer treatment.

  12. An airborne actinobacteria Nocardiopsis alba isolated from bioaerosol of a mushroom compost facility.

    PubMed

    Paściak, Mariola; Pawlik, Krzysztof; Gamian, Andrzej; Szponar, Bogumiła; Skóra, Justyna; Gutarowska, Beata

    2014-01-01

    Actinobacteria are widely distributed in many environments and represent the most important trigger to the occupant respiratory health. Health complaints, including hypersensitivity pneumonitis of the workers, were recorded in a mushroom compost facility (MCF). The studies on the airborne bacteria were carried out to find a possible microbiological source of these symptoms. Culture analysis of compost bioaerosols collected in different location of the MCF was performed. An assessment of the indoor microbial exposure revealed bacterial flora of bioaerosol in the mushroom compost facility represented by Bacillus, Geobacillus, Micrococcus, Pseudomonas, Staphylococcus spp., and actinobacterial strain with white aerial mycelium. The thermotolerant actinobacterial strain of the same morphology was repeatedly isolated from many locations in MCF: air, compost sample, and solid surface in production hall. On the base of complex morphological, chemotaxonomic, and phylogenetic characteristics, the isolate has been classified as Nocardiopsis alba. Dominant position of N. alba in microbial environment of the mushroom compost facility may represent an indicator microorganism in compost bioaerosol. The bioavailability of N. alba in mushroom compost facility creates potential risk for the health of workers, and the protection of respiratory tract and/or skin is strongly recommended.

  13. The Mars Climate Sounder on the Mars Reconnaissance Orbiter

    NASA Astrophysics Data System (ADS)

    McCleese, D.; Taylor, F.; Schofield, J.; Calcutt, S.

    2003-04-01

    There remains a need for an intensive effort to obtain a climatology of the martian atmosphere. This objective was to have been accomplished with the Mars Observer and with the Mars Climatology Orbiter, both of which failed at Mars. In 2005, the Mars Reconnaissance Orbiter will carry the Mars Climate Sounder (MCS) to aquire the necessary measurements of the vertical profiles of atmospheric temperature, water vapor, dust and condensates. This paper describes the climate objectives and measurement approach of MCS.

  14. Mars Aerobot Validation Program

    NASA Technical Reports Server (NTRS)

    Kerzhanovich, V. V.; Cutts, J.; Bachelder, A.; Cameron, J.; Patzold, J.; Quadrelli, M.; Yavrouian, A.; Cantrell, J.; Lachenmeier, T.; Smith, M.

    1999-01-01

    The Mars Balloon Validation Program (MABVAP) was initiated in August 1997 to develop and validate key technologies needed for aerobot missions on Mars. The major elements of the program are the development of balloons for flight on Mars, robust techniques for deployment and inflation and modeling and simulation of balloon flight paths. selection, development and tests of available balloon materials, design and fabrication of balloons (both superpressure and solar- heated), design and fabrication of deployment and inflation systems for aerial deployment, design and fabrication of avionics to control deployment/inflation process and to get telemetry and video data. Modeling of main processes during deployment and actual flight is also a part of MABVAP. In order to validate deployment and inflation, MABVAP applies experience from previous Mars balloon development or study activities the Russian-French Mars Aerostat Project (1988-1995), Mars Aerial Platform Study (1994) and Mars Aerobot/Balloon Study (1996). The program includes laboratory, wind tunnel, vacuum chamber tests of the system components and a number of tropospheric and stratospheric flight tests of deployment and inflation of lightfilm balloons in a simulated Martian environment.

  15. Pebbles on Mars

    NASA Astrophysics Data System (ADS)

    Jerolmack, Douglas J.

    2013-05-01

    Mars is a cold, dry place. Yet there is abundant evidence that fluvial (river) processes have carved the planet's surface; witness deep canyons, streamlined islands, and drainage networks. Most of these features formed more than 3 billion years ago, and a long line of research has led to the "warm and wet early Mars" hypothesis. The idea is that early Mars had a thicker atmosphere with an enhanced greenhouse effect that allowed stable liquid water and a hydrologic cycle to exist. The search for life on Mars, or at least conditions suitable for life, is predicated on this idea. Until now, no observations have unambiguously identified and characterized river-lain sediments, although the Mars Exploration Rovers turned up some evidence of a watery past. As the first major finding from the Mars Science Laboratory mission and its car-sized rover, Curiosity, Williams et al. report on page 1068 of this issue the discovery of conglomerates on Mars - pebbles mixed with sand and turned to rock - resulting from ancient river deposits. The finding provides the clearest view yet on the nature of early martian rivers and should provide momentum for Curiosity's mission moving forward.

  16. ExoMars 2016 arrives at Mars

    NASA Astrophysics Data System (ADS)

    Svedhem, Hakan; Vago, Jorge L.; ExoMars Team

    2016-10-01

    The Trace Gas Orbiter (TGO) and the Schiaparelli Entry, descent and landing Demonstrator Model (EDM) will arrive at Mars on 19 October 2016. The TGO and the EDM are part of the first step of the ExoMars Programme. They will be followed by a Rover and a long lived Surface Platform to be launched in 2020.The EDM is attached to the TGO for the full duration of the cruise to Mars and will be separated three days before arrival at Mars. After separation the TGO will perform a deflection manoeuvre and, on 19 October (during the EDM landing), enter into a highly elliptical near equatorial orbit. TGO will remain in this parking orbit until January 2017, when the orbital plane inclination will be changed to 74 degrees and aerobraking to the final 400 km near circular orbit will start. The final operational orbit is expected to be reached at the end of 2017.The TGO scientific payload consists of four instruments. These are: ACS and NOMAD, both infrared spectrometers for atmospheric measurements in solar occultation mode and in nadir mode, CASSIS, a multichannel camera with stereo imaging capability, and FREND, an epithermal neutron detector for search of subsurface hydrogen. The mass of the TGO is 3700 kg, including fuel. The EDM, with a mass of 600 kg, is mounted on top of the TGO as seen in its launch configuration. The main objective of the EDM is to demonstrate the capability of performing a safe entry, descent and landing on the surface, but it does carry a descent camera and a small battery powered meteorological package that may operate for a few days on the surface.The ExoMars programme is a joint activity by the European Space Agency(ESA) and ROSCOSMOS, Russia. ESA is providing the TGO spacecraft and Schiaparelli (EDM) and two of the TGO instruments and ROSCOSMOS is providing the launcher and the other two TGO instruments. After the arrival of the ExoMars 2020 mission at the surface of Mars, the TGO will handle the communication between the Earth and the Rover and

  17. Third International Colloquium on Mars

    NASA Technical Reports Server (NTRS)

    1981-01-01

    Abstracts of papers concerning the geology and geophysics of Mars, volcanism on Mars, the Mars atmosphere, and the long term history of the atmosphere-cap-regolith volatile regime are presented. Formation of the Mars surface, climatology, gravity and magnetism, atmospheric boundary layers, and interpretation of Viking imagery and Earth-based observations are considered.

  18. Ignimbrites of Amazonis Planitia region of Mars

    NASA Technical Reports Server (NTRS)

    Scott, D. H.; Tanaka, K. L.

    1982-01-01

    The terms ignimbrite and ash flow tuff are used to describe relatively thin but extensive sheets of material interpreted to be of pyroclastic origin and to consist of volcanic ash or pumice fragments. Criteria for distinguishing ignimbrites from other geologic materials are considered, and characteristics observed for rock units interpreted as ignimbrites in Amazonis Planitia are discussed. A series of rock units which are thought to represent ignimbrites have been mapped along an east-west border zone between the highland plateau and lowland plains of Amazonis Planitia. The area is roughly bounded by a triangle whose apices are the volcanoes Apollinaris Patera, Biblis Patera, and Olympus Mons. Attention is given to aspects of general geology, morphology and stratigraphy, and thickness and volume estimates. Correlations with other data are considered and some theoretical aspects of Martian ignimbrite emplacement are discussed.

  19. Mars Observer's costly solitude

    NASA Astrophysics Data System (ADS)

    Travis, John

    1993-09-01

    An evaluation is presented of the ramifications of the loss of contact with the Mars Observer spacecraft in August, 1993; the Observer constituted the first NASA mission to Mars in 17 years. It is noted that most, if not all of the scientists involved with the mission will have to find alternative employment within 6 months. The loss of the Observer will leave major questions concerning the geologic history of Mars, and its turbulent atmospheric circulation, unanswered. A detailed account of the discovery of the loss of communications, the unsuccessful steps taken to rectify the problem, and the financial losses incurred through the failure of the mission, are also given.

  20. Mars surface transportation options

    NASA Technical Reports Server (NTRS)

    Leitner, Jeffrey M.; Alred, John W.

    1986-01-01

    As the number of scientific experiments for the surface of Mars grows, the need for effective surface transportation becomes critical. Because of the diversity of the experiments proposed, as well as the desire to explore Mars from the equator to the poles, the optimum surface vehicle configuration is not obvious. Five candidate vehicles are described, with an estimate of their size and performance. In order to maximize the success of a manned Mars mission, it appears that two vehicles should be designed for surface transportation: an advanced long-range rover, and a remotely-piloted airplane.

  1. Life on Mars

    NASA Technical Reports Server (NTRS)

    Soffen, G. A.

    1981-01-01

    The Viking biology experiments are examined. It is noted that the Viking missions did not find a terrestrial type of life at either of the two landing sites. This evidence may suggest that Mars is lifeless, but science demands a more rigorous proof; thus, it is still not known whether life exists on Mars. It is suggested that the Martian polar regions must be explored before a conclusive answer is possible; the permanent polar caps of Mars are frozen water and would act as a 'cold finger' of the planet to trap organic molecules.

  2. The Mars observer camera

    NASA Technical Reports Server (NTRS)

    Malin, M. C.; Danielson, G. E.; Ingersoll, A. P.; Masursky, H.; Veverka, J.; Soulanille, T.; Ravine, M.

    1987-01-01

    A camera designed to operate under the extreme constraints of the Mars Observer Mission was selected by NASA in April, 1986. Contingent upon final confirmation in mid-November, the Mars Observer Camera (MOC) will begin acquiring images of the surface and atmosphere of Mars in September-October 1991. The MOC incorporates both a wide angle system for low resolution global monitoring and intermediate resolution regional targeting, and a narrow angle system for high resolution selective surveys. Camera electronics provide control of image clocking and on-board, internal editing and buffering to match whatever spacecraft data system capabilities are allocated to the experiment. The objectives of the MOC experiment follow.

  3. Mars Aerocapture Systems Study

    NASA Technical Reports Server (NTRS)

    Wright, Henry S.; Oh, David Y.; Westhelle, Carlos H.; Fisher, Jody L.; Dyke, R. Eric; Edquist, Karl T.; Brown, James L.; Justh, Hilary L.; Munk, Michelle M.

    2006-01-01

    Mars Aerocapture Systems Study (MASS) is a detailed study of the application of aerocapture to a large Mars robotic orbiter to assess and identify key technology gaps. This study addressed use of an Opposition class return segment for use in the Mars Sample Return architecture. Study addressed mission architecture issues as well as system design. Key trade studies focused on design of aerocapture aeroshell, spacecraft design and packaging, guidance, navigation and control with simulation, computational fluid dynamics, and thermal protection system sizing. Detailed master equipment lists are included as well as a cursory cost assessment.

  4. Human Exploration of Mars

    NASA Astrophysics Data System (ADS)

    Gwynne, Owen; McKay, Chris; Zubrin, Robert

    1991-06-01

    Novel approaches to the human exploration of Mars are considered with emphasis on a space suit design, extraterrestrial surface mobility, and water supply. A possible way of transporting personnel on the surface of Mars uses a suborbital rocket that will hop from one site to the next, refuelling each time it lands and giving the Martian explorers effective global mobility. Telepresence could be used to avoid limiting the people on Mars to a small exploration area as a result of a lack of transportation infrastructure. Drawings and photographs are included.

  5. Water on Mars

    NASA Technical Reports Server (NTRS)

    Waenke, H.; Dreibus, G.

    1987-01-01

    It is reported that the SNC meteorites are a factor of 2 richer in moderately volatile elements (Na, K, P, etc.) and some volatile elements (Cl, Br, I, S) compared to the Earth and Mars. It is proposed that Mars accreted homogeneously, with the result that all the water except trace amounts (on reaction with metallic Fe) was converted to H(sub 2) and escaped. This model predicts a total Mars H(sub 2)O inventory of 18 ppm (equivalent to an ocean 80 m deep on the planet), and a value for Earth of 300 ppm, close to the actual abundance.

  6. Airbag Tracks on Mars

    NASA Technical Reports Server (NTRS)

    2004-01-01

    The circular shapes seen on the martian surface in these images are 'footprints' left by the Mars Exploration Rover Opportunity's airbags during landing as the spacecraft gently rolled to a stop. Opportunity landed at approximately 9:05 p.m. PST on Saturday, Jan. 24, 2004, Earth-received time. The circular region of the flower-like feature on the right is about the size of a basketball. Scientists are studying the prints for more clues about the makeup of martian soil. The images were taken at Meridiani Planum, Mars, by the panoramic camera on the Mars Exploration Rover Opportunity.

  7. Mars tectonics and volcanism

    NASA Technical Reports Server (NTRS)

    Solomon, Sean C.

    1990-01-01

    The focus of this research was on three broad areas: (1) the relation between lithospheric stress in the vicinity of a growing volcano and the evolution of eruption characteristics and tectonic faulting; (2) the relation between elastic lithosphere thickness and thermal structure; and (3) a synthesis of constraints on heat flow and internal dynamics on Mars. The two reports presented are: (1) Heterogeneities in the Thickness of the Elastic Lithosphere of Mars--Constraints on Heat Flow and Internal Dynamics; and (2) State of Stress, Faulting, and Eruption Characteristics of Large Volcanoes on Mars.

  8. Exobiology on Mars

    NASA Technical Reports Server (NTRS)

    Devincenzi, D. L. (Editor); Marshall, J. R. (Editor); Andersen, D. (Editor)

    1990-01-01

    Descriptions of several instrument concepts that were generated during a workshop entitled, Exobiology Instrument Concepts for a Soviet Mars 94/94 Mission, held at NASA Ames Research Center in 1989 are presented. The objective was to define and describe instrument concepts for exobiology and related science that would be compatible with the mission types under discussion for the 1994 and 1996 Soviet Mars missions. Experiments that use existing technology were emphasized. The concepts discussed could also be used on U.S. missions that follow Mars Observer.

  9. Mars Equipment Transport System

    NASA Technical Reports Server (NTRS)

    Sorrells, Cindy; Geiger, Michelle; Ohanlon, Sean; Pieloch, Stuart; Brogan, Nick

    1993-01-01

    Mechanical Engineering Senior Design Project 1 (ME4182) is a part of the NASA/University Advanced Design Program. Under this program, NASA allocates money and resources to students to be used in design work for a specified topic. The current topic is the exploration and colonization of Mars. The specific area in which we are to work is the transportation of the modules in which astronauts will live while on Mars. NASA is concerned about the weight of the module transferring system, as the shipping cost to Mars is quite expensive. NASA has specified that the weight of the system is to be minimized in order to reduce the shipping costs.

  10. Geology and landscape evolution of the Hellas region of Mars

    NASA Technical Reports Server (NTRS)

    Tanaka, Kenneth L.; Leonard, Gregory J.

    1995-01-01

    Hellas basin on Mars has been the site of volcanism, tectonism, and modification by fluvial, mass-wasting, and eolian processes over its more than 4-b.y. existence. Our detailed geologic mapping and related studies have resulted in the following new interpretations. The asymmetric distribution of highland massifs and other structures that define the uplifted basin rim suggest a formation of the basin by the impact of a low-angle bolide having a trajectory heading S 60 deg E. During the Late Noachian, the basin was infilled, perhaps by lava flows, that were sufficiently thick (>1 km) to produce wrinkle ridges on the fill material and extensional faulting along the west rim of the basin. At about the same time, deposits buried northern Malea Planum, which are interpreted to be pyroclastic flows from Amphitrites and Peneus Paterae on the basis of their degraded morphology, topography, and the application of a previous model for pyroclastic volcanism on Mars. Peneus forms a distinctive caldera structure that indicates eruption of massive volumes of magma, whereas Amphitrites is a less distinct circular feature surrounded by a broad, low, dissected shield that suggests generally smaller volume eruptions. During the Early Hesperian, an approx. 1- to 2-km-thick sequence of primarily fined-grained, eolian material was deposited on the floor of Hellas basin. Subsequently, the deposit was deeply eroded, except where armored by crater ejecta, and it retreated as much as 200-300 km along its western margin, leaving behind pedestal craters and knobby outliers of the deposit. Local debris flows within the deposit attest to concentrations of groundwater, perhaps in part brought in by outflow floods along the east rim of the basin. These floods may have deposited approx. 100-200 m of sediment, subduing wrinkle ridges in the eastern part of the basin floor. During the Late Hesperian and Amazonian, eolian mantles were emplaced on the basin rim and floor and surrounding highlands

  11. Geology and landscape evolution of the Hellas region of Mars

    NASA Technical Reports Server (NTRS)

    Tanaka, Kenneth L.; Leonard, Gregory J.

    1995-01-01

    Hellas basin on Mars has been the site of volcanism, tectonism, and modification by fluvial, mass-wasting, and eolian processes over its more than 4-b.y. existence. Our detailed geologic mapping and related studies have resulted in the following new interpretations. The asymmetric distribution of highland massifs and other structures that define the uplifted basin rim suggest a formation of the basin by the impact of a low-angle bolide having a trajectory heading S60E. During the Late Noachian, the basin was infilled, perhaps by lava flows, that were sufficiently thick (greater than 1 km) to produce wrinkle ridges on the fill material and extensional faulting along the west rim of the basin. At about the same time, deposits buried northern Malea Planum, which are interpreted to be pyroclastic flows from Amphitrites and Peneus Paterae on the basis of their degraded morphology, topology, and the application of a previous model for pyroclastic volcanism on Mars. Peneus forms a distinctive caldera structure that indicates eruption of massive volumes of magma, whereas Amphitrites is a less distinct circular feature surrounded by a broad, low, dissected shield that suggests generally smaller volume eruptions. During the Early Hesperian, an approximately 1-to 2km-thick sequence of primarily fined-grained, eolian material was deposited on the floor of Hellas basin. Subsequently, the deposit was deeply eroded, except where armored by crater ejecta, and it retreated as much as 200-300 km along its western margin, leaving behind pedestal craters and knobby outliers of the deposit. Local debris flows within the deposit attest to concentrations of groundwater, perhaps in part brought in by outflow floods along the east rim of the basin. These floods may have deposited approximately 100-200m of sediment, subduing wrinkle ridges in the eastern part of the basin floor. During the Late Hesperian and Amazonian, eolian mantles were emplaced on the basin rim and floor and surrounding

  12. The influence of phosphorus nutritional status on the uptake of germanium in Panicum miliaceum and Brassica alba

    NASA Astrophysics Data System (ADS)

    Kaden, Ute Susanne; Székely, Balázs; Wiche, Oliver

    2015-04-01

    In order to investigate the influence of the phosphorus nutritional status on the uptake of germanium (Ge) in biomass two species, white millet (Panicum miliaceum) and white mustard (Brassica alba) were grown and sampled in a greenhouse experiment. The cultivation took place on two different substrates. The plants were fertilized with different nutrient solutions which differed in their phosphate content, and artificial addition of Ge was held via the casting solution. During the test period, measurements of the pH value, electric conductivity, and phosphate content of the soil solution were conducted. To transfer germanium from soil and plant material in solution, melting and microwave digestion processes were done. The experiment showed that in both species the additional Ge supply also leads to an increasing germanium content in the aboveground plant material. The two species, however, behave differently in response to this Ge supply. Panicum miliaceum accumulates Ge in the above-ground parts of plants stem, leaf and fruit to a much greater extent than Brassica alba. On the other hand the Ge accumulation in the roots of both B. alba and P. miliaceum was very high. In case of B. alba the root content was found by far higher as compared to the other parts of the plant. The addition of phosphate in the system changes the behavior. Without additional Ge its natural uptake from soil decreases in both species but in B. alba it is more characteristic. Increasing Ge supply (for both species) leads to an increased Ge uptake, until it reaches a maximum, regardless of the presence of phosphate addition. Phosphate, on the other hand, has positive effects on Ge uptake only in the case of B. alba roots, and to a limited extent in roots of P. miliaceum. In addition, for Panicum miliaceum an increase of germanium mainly in the underground parts was achieved. A further addition of phosphate did not have a positive effect on a greater enrichment of germanium. Whereas in Brassica

  13. NASA's Mars Landings

    NASA Video Gallery

    This video shows the landing sites of all six NASA spacecraft to reachMars—Viking 1, Viking 2, Pathfinder, Spirit, Opportunity, Phoenix—and thetarget location where Curiosity will touch down ...

  14. Bringing Life to Mars

    NASA Technical Reports Server (NTRS)

    McKay, C. P.

    1999-01-01

    A suitable long-term goal for human exploration of Mars is the determination of whether or not a self-sustainable bio-sphere could be constructed on Mars, a process called Terraforming. Preliminary considerations of the conditions on a habitable Mars suggest that there are two potentially habitable states: one -characterized by an atmosphere of 1-3 bars of CO2 - would be habitable for plants and microorganisms and another which would be habitable by humans. It may be possible to warm the planet by selective introduction of trace gases to enhance the greenhouse effect. Energy balance considerations suggest that warming Mars would take on the order of 100 years with a much longer time required to produce a breathable atmosphere.

  15. Mars Exploration Rover Mission

    NASA Technical Reports Server (NTRS)

    Cohen, Barbara A.

    2008-01-01

    This viewgraph presentation reviews the Mars Exploration Rover Mission. The design of the Rover along with the Athena science payload is also described. Photographs of the Gusev Crater and Meridiani rocks are also shown.

  16. Environment of Mars, 1988

    NASA Technical Reports Server (NTRS)

    Kaplan, David I. (Compiler)

    1988-01-01

    A compilation of scientific knowledge about the planet Mars is provided. Information is divided into three categories: atmospheric data, surface data, and astrodynamic data. The discussion of atmospheric data includes the presentation of nine different models of the Mars atmosphere. Also discussed are Martian atmospheric constituents, winds, clouds, and solar irradiance. The great dust storms of Mars are presented. The section on Mars surface data provides an in-depth examination of the physical and chemical properties observed at the two Viking landing sites. Bulk densities, dielectric constants, and thermal inertias across the planet are then described and related back to those specific features found at the Viking landing sites. The astrodynamic materials provide the astronomical constants, time scales, and reference coordinate frames necessary to perform flightpath analysis, navigation design, and science observation design.

  17. Mars Balance Challenge

    NASA Video Gallery

    The Challenge is to develop ideas for how NASA can turn available entry, descent, and landing balance mass on a future Mars mission into a scientific or technological payload. Proposed concepts sho...

  18. Explore Mars With Curiosity

    NASA Video Gallery

    This animation shows the approximate true position of NASA’s Curiosityrover on Mars. A 3-D virtual model of Curiosity is shown inside GaleCrater, near Mount Sharp, Curiosity’s ultimate destin...

  19. Interactive Science on Mars

    NASA Astrophysics Data System (ADS)

    Mercer, C. R.; Landis, G. A.

    2017-02-01

    Swarms of small citizen-driven rovers can conduct Mars surface science missions. Transportation and communication technology needed for human exploration can enable this new interactive science mission architecture.

  20. Mars Exploration Zones

    NASA Video Gallery

    This concept animation shows just one of many potential concepts for how the first human landing site on Mars might evolve throughout the course of multiple human expeditions to the Red Planet over...

  1. Mars Acoustic Anemometer

    NASA Astrophysics Data System (ADS)

    Banfield, D. J.

    2012-12-01

    We have developed a very high performance anemometer (wind gauge) for use at Mars. This instrument has great scientific as well as strategic reasons to be included on all future missions to the surface of Mars. We will discuss why we set out to develop this instrument, as well as why the previous wind sensors for Mars are insufficient to meet the scientific and strategic needs at Mars. We will also discuss how the instrument works, and how it differs from terrestrial counterparts. Additionally, we will discuss the current status of the instrument. Measuring winds at Mars is important to better understand the atmospheric circulation at Mars, as well as exchange between the surface and atmosphere. The main conduit of transport of water, and hence its current stability at any particular location on Mars is controlled by these atmospheric motions and the exchange between surface and atmosphere. Mars' large-scale winds are moderately well understood from orbital observations, but the interaction with the surface can only be addressed adequately in situ. Previous anemometers have been 2-D (with the exception of REMS on MSL) and slow response (typically <1Hz), and relatively low sensitivity/accuracy (>1 m/s). Our instrument is capable of fully 3-D measurements, with fast response (>20 Hz) and great sensitivity/accuracy (~3 cm/s). This significant step forward in performance is important for the surface-atmosphere exchanges of heat, momentum and volatiles. In particular, our instrument could directly measure the heat and momentum fluxes between surface and atmosphere using eddy-flux techniques proven terrestrially. When combined with a fast response volatile analysis instrument (e.g., a TLS) we can also measure eddy fluxes of volatile transport. Such a study would be nearly impossible to carry out with preceding anemometers sent to Mars with insufficient response time and sensitivity to adequately sample the turbulent eddies. Additionally, our instrument, using acoustics

  2. Mars Analytical Laboratory

    NASA Astrophysics Data System (ADS)

    Nagati, M. Gawad; Ale-Ibrahaim, Kordi; Bins, Llonda; Davis, Michael; Gamalo, Johnny; Johnson, Matt; May, Neal; Seneviratne, Waruna; Yurko, Aric; Yurko, Brenda

    1998-01-01

    As mankind continues to explore the solar system, planetary colonization may become an important goal. Permanently manned space stations, bases on the moon, and colonization of Mars will be important steps in this exploration. The colonization and exploration of Mars will be a particular challenge. As mankind one day attempts this colonization, knowledge of the Martian environment and human capacity to live there will become vitally important. The first scientific outposts on Mars will need research laboratories to make discoveries about how we can better live there and use the natural resources of the planet to sustain human life. The design of a laboratory for an existing Martian base is the purpose of this project. A laboratory on Mars would be very useful to the scientists we send.

  3. Internal constitution of Mars.

    NASA Technical Reports Server (NTRS)

    Anderson, D. L.

    1972-01-01

    Models of the internal structure of Mars consistent with the mass, radius and moment of inertia of the planet are constructed. The models assume that the radius of the core is between 0.36 and 0.60 of the radius of the planet, that the zero-pressure density of the mantle is between 3.54 and 3.49 g/cu cm, and that the planet contains 25 to 28% iron. Meteorite models of Mars containing 25 wt % iron and 12 wt % core are also proposed. It is maintained that Mars in contrast to the earth is an incompletely differentiated planet with a core substantially richer in sulfur than the core of the earth. The absence of a magnetic field on Mars is possibly linked with lack of lunar precessional torque and the small size and high resistivity of the Martian core.

  4. Methane Plumes on Mars

    NASA Video Gallery

    Spectrometer instruments attached to several telescopes detect plumes of methane emitted from Mars during its summer and spring seasons. High levels of methane are indicated by warmer colors. The m...

  5. Airbag Deflates on Mars

    NASA Technical Reports Server (NTRS)

    2004-01-01

    This image, taken by the navigation camera onboard the Mars Exploration Rover Spirit, shows the airbags used to protect the rover during landing. One bright, dust-covered bag is slightly puffed up against the lander.

  6. The Cruise to Mars

    NASA Video Gallery

    The long journey to Mars through the harsh environment of spaceconfronts the Curiosity navigation team with a long list of challengesto get the spacecraft safely to its destination.› Mission site

  7. Mars exploration program

    NASA Technical Reports Server (NTRS)

    Weary, Dwayne

    1993-01-01

    An overview of the Mars Exploration Program is presented in outline and graphic form. Mission objectives, mission strategy, operations concept, transportation element, launch vehicle considerations and program schedule are addressed.

  8. Wind abrasion on Mars

    NASA Technical Reports Server (NTRS)

    Greeley, Ronald

    1991-01-01

    Aeolian activity was predicted for Mars from earth based observations of changing surface patterns that were interpreted as dust storms. Mariner 9 images showed conclusive evidence for aeolian processes in the form of active dust storms and various aeolian landforms including dunes and yardangs. Windspeeds to initiate particle movement are an order of magnitude higher on Mars than on Earth because of the low atmospheric density on Mars. In order to determine rates of abrasion by wind blown particles, knowledge of three factors is required: (1) particle parameters such as numbers and velocities of windblown grains as functions of windspeeds at various heights above the surface; (2) the susceptibility to abrasion of various rocks and minerals; and (3) wind frequencies and speeds. For estimates appropriate to Mars, data for the first two parameters can be determined through lab and wind tunnel tests; data for the last two factors are available directly from the Viking Lander meteorology experiments for the two landing sites.

  9. Effects of phytohormones and jasmonic acid on glucosinolate content in hairy root cultures of Sinapis alba and Brassica rapa.

    PubMed

    Kastell, Anja; Smetanska, Iryna; Ulrichs, Christian; Cai, Zhenzhen; Mewis, Inga

    2013-01-01

    Although some study have established hairy root cultures from brassicaceous plants with glucosinolates (GS) as characteristic secondary metabolite, studies are missing which compare hairy roots with the corresponding mother plants. Therefore, two different plant species-Sinapis alba and Brassica rapa subsp. rapa pygmeae teltoviensis-were transformed with the Agrobacterium rhizogenes strain A4. Aliphatic and indolyl GS were present in B. rapa, exhibiting larger quantities in leaves than in roots. Aromatic p-hydroxybenzyl GS were found particularly in the leaves of S. alba. However, the proportion of indolyl GS increased suddenly in transformed hairy roots of S. alba and B. rapa. Cultivation with the phytohormone kinetin (0.5 mg L(-1)) enhanced GS accumulation in B. rapa hairy roots, however not in S. alba, but 2,4-D (0.4 mg L(-1)) induced de-differentiation of roots in both species and reduced GS levels. GS levels especially of 1-methoxyindol-3ylmethyl GS increased in hairy roots in response to JA, but root growth was inhibited. While 2 weeks of cultivation in 100 to 200 μM JA were determined at optimum for maximum GS yield in S. alba hairy root cultures, 4 weeks of cultivation in 50 to 100 μM JA was the optimum for B. rapa.

  10. Asteraceae Artemisia campestris and Artemisia herba-alba Essential Oils Trigger Apoptosis and Cell Cycle Arrest in Leishmania infantum Promastigotes

    PubMed Central

    Messaoud, Chokri; Haoues, Meriam; Neffati, Noura; Bassoumi Jamoussi, Imen; Essafi-Benkhadir, Khadija; Boussaid, Mohamed; Karoui, Habib

    2016-01-01

    We report the chemical composition and anti-Leishmania and antioxidant activity of Artemisia campestris L. and Artemisia herba-alba Asso. essential oils (EOs). Our results showed that these extracts exhibit different antioxidant activities according to the used assay. The radical scavenging effects determined by DPPH assay were of IC50 = 3.3 mg/mL and IC50 = 9.1 mg/mL for Artemisia campestris and Artemisia herba-alba essential oils, respectively. However, antioxidant effects of both essential oils, determined by ferric-reducing antioxidant power (FRAP) assay, were in the same range (2.3 and 2.97 mg eq EDTA/g EO, resp.), while the Artemisia herba-alba essential oil showed highest chelating activity of Fe2+ ions (27.48 mM Fe2+). Interestingly, we showed that both EOs possess dose-dependent activity against Leishmania infantum promastigotes with IC50 values of 68 μg/mL and 44 μg/mL for A. herba-alba and A. campestris, respectively. We reported, for the first time, that antileishmanial activity of both EOs was mediated by cell apoptosis induction and cell cycle arrest at the sub-G0/G1 phase. All our results showed that EOs from A. herba-alba and A. campestris plants are promising candidates as anti-Leishmania medicinal products. PMID:27807464

  11. Chemical variability of essential oils of Lippia alba (Miller) N. E. Brown growing in Costa Rica and Argentina.

    PubMed

    Ricciardi, Gabriela; Cicció, José F; Ocampo, Rafael; Lorenzo, Daniel; Ricciardi, Armando; Bandoni, Arnaldo; Dellacassa, Eduardo

    2009-06-01

    Lippia alba (Verbenaceae) is a shrub whose essential oil has important biological, pharmacological, and aromatizing properties. The species has a natural range from Central America to Argentina, being cultivated for its commercial value in Brazil, Argentina and Guatemala, and has been introduced into India and Spain. To reach the economic potential of the plant, the present study was aimed at evaluating L. alba for different chemotypes. The composition of the essential oil from two native populations of L. alba, collected from Argentina and two accessions from Costa Rica, were screened by GC and GC-MS. The results obtained led us to adopt the concept of a biodistribution map, as was proposed previously for the species, representing an approach to the natural biological distribution of the species in America based on the chemotypes described and their geographical distribution. Moreover, the biodiversity reported for the species (seven of eight chemotypes described for L. alba are present in Argentina) suggests the southern region of South America as the centre of distribution for L. alba.

  12. Water on Mars

    USGS Publications Warehouse

    Carr, M.H.

    1987-01-01

    Estimates of the amount of water outgassed from Mars, based on the composition of the atmosphere, range from 6 to 160 m, as compared with 3 km for the Earth. In contrast, large flood features, valley networks, and several indicators of ground ice suggest that at least 500 m of water have outgassed. The two sets of estimates may be reconciled if early in its history, Mars lost part of its atmosphere by impact erosion and hydrodynamic escape. ?? 1987 Nature Publishing Group.

  13. Mars Ice Age, Simulated

    NASA Technical Reports Server (NTRS)

    2003-01-01

    December 17, 2003

    This simulated view shows Mars as it might have appeared during the height of a possible ice age in geologically recent time.

    Of all Solar System planets, Mars has the climate most like that of Earth. Both are sensitive to small changes in orbit and tilt. During a period about 2.1 million to 400,000 years ago, increased tilt of Mars' rotational axis caused increased solar heating at the poles. A new study using observations from NASA's Mars Global Surveyor and Mars Odyssey orbiters concludes that this polar warming caused mobilization of water vapor and dust into the atmosphere, and buildup of a surface deposit of ice and dust down to about 30 degrees latitude in both hemispheres. That is the equivalent of the southern Unites States or Saudi Arabia on Earth. Mars has been in an interglacial period characterized by less axial tilt for about the last 300,000 years. The ice-rich surface deposit has been degrading in the latitude zone of 30 degrees to 60 degrees as water-ice returns to the poles.

    In this illustration prepared for the December 18, 2003, cover of the journal Nature, the simulated surface deposit is superposed on a topography map based on altitude measurements by Global Surveyor and images from NASA's Viking orbiters of the 1970s.

    Mars Global Surveyor and Mars Odyssey are managed by NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, for the NASA Office of Space Science, Washington.

  14. Status of MARS Code

    SciTech Connect

    N.V. Mokhov

    2003-04-09

    Status and recent developments of the MARS 14 Monte Carlo code system for simulation of hadronic and electromagnetic cascades in shielding, accelerator and detector components in the energy range from a fraction of an electronvolt up to 100 TeV are described. these include physics models both in strong and electromagnetic interaction sectors, variance reduction techniques, residual dose, geometry, tracking, histograming. MAD-MARS Beam Line Build and Graphical-User Interface.

  15. Mars Gravity Anomoly Map

    NASA Technical Reports Server (NTRS)

    2001-01-01

    This is a vertical gravity map of Mars color-coded in mgals based on radio tracking. Note correlations and lack of correlations with the Mars Orbiter Laser Altimeter (MOLA) global topography.

    This map was created using MGS data under the direction of Bill Sjogren, a member of the MGS Radio Science Team. The Radio Science Team is led by G. Leonard Tyler of Stanford University in Palo Alto, CA.

  16. A Mars 1984 mission

    NASA Technical Reports Server (NTRS)

    1977-01-01

    Mission objectives are developed for the next logical step in the investigation of the local physical and chemical environments and the search for organic compounds on Mars. The necessity of three vehicular elements: orbiter, penetrator, and rover for in situ investigations of atmospheric-lithospheric interactions is emphasized. A summary report and committee recommendations are included with the full report of the Mars Science Working Group.

  17. Clouds over Mars!

    NASA Technical Reports Server (NTRS)

    1997-01-01

    This is the first color image ever taken from the surface of Mars of an overcast sky. Featured are pink stratus clouds coming from the northeast at about 15 miles per hour (6.7 meters/second) at an approximate height of ten miles (16 kilometers) above the surface. The clouds consist of water ice condensed on reddish dust particles suspended in the atmosphere. Clouds on Mars are sometimes localized and can sometimes cover entire regions, but have not yet been observed to cover the entire planet. The image was taken about an hour and forty minutes before sunrise by the Imager for Mars Pathfinder (IMP) on Sol 16 at about ten degrees up from the eastern Martian horizon.

    Mars Pathfinder is the second in NASA's Discovery program of low-cost spacecraft with highly focused science goals. The Jet Propulsion Laboratory, Pasadena, CA, developed and manages and Mars Pathfinder mission for NASA's Office of Space Science, Washington, D.C. JPL is an operating division of the California Institute of Technology (Caltech). The Imager for Mars Pathfinder (IMP) was developed by the University of Arizona Lunar and Planetary Laboratory under contract to JPL. Peter Smith is the Principal Investigator.

  18. Transportation: Destination Mars

    NASA Technical Reports Server (NTRS)

    Eoff, Bill

    1998-01-01

    As the agency space transportation lead center, Marshall Space Flight Center has been conducting transportation assessments for future robotic and human Mars missions to identify critical technologies. Five human Mars options are currently under assessment with each option including all transportation requirements from Earth to Mars and return. The primary difference for each option is the propulsion source from Earth to Mars. In case any of the options require heavy launch capability that is not currently projected as available, an in-house study has been initiated to determine the most cost effective means of providing such launch capability. This assessment is only considering launch architectures that support the overall human Mars mission cost goal of $25B. The guidelines for the launch capability study included delivery of 80 metric ton (176 KLB) payloads, 25 feet diameter x 92 feet long, to 220 nmi orbits at 28.5 degrees. The launch vehicle concept of the study was designated "Magnum" to differentiate from prior heavy launch vehicle assessments. This assessment along with the assessment of options for all transportation phases of a Mars mission are on-going.

  19. Life on Mars

    NASA Technical Reports Server (NTRS)

    McKay, Christopher P.; Cuzzi, Jeffrey (Technical Monitor)

    1996-01-01

    Although the Viking results may indicate that Mars has no life today, the possibility exists that Mars may hold the best record of the events that led to the origin of life. There is direct geomorphological evidence that in the past Mars had large amounts of liquid water on its surface. Atmospheric models would suggest that this early period of hydrological activity was due to the presence of a thick atmosphere and the resulting warmer temperatures. From a biological perspective the existence of liquid water, by itself motivates the question of the origin of life on Mars. From studies of the Earth's earliest biosphere we know that by 3.5 Gyr. ago, life had originated on Earth and reached a fair degree of biological sophistication. Surface activity and erosion on Earth make it difficult to trace the history of life before the 3.5 Gyr timeframe. If Mars did maintain a clement environment for longer than it took for life to originate on Earth, then the question of the origin of life on Mars follows naturally.

  20. Modern myths of Mars

    NASA Astrophysics Data System (ADS)

    Levin, Gilbert V.

    2006-08-01

    July 30, 2006 was the 30 th anniversary of the Viking Mission's first Labeled Release (LR) life detection experiment on Mars. The strong response, together with supporting results from eight additional LR tests of Martian soil, established the presence of an active agent that was inhibited by heating. The data satisfied the pre-mission criteria for the detection of living microorganisms. However, the scientific community reacted cautiously, generally concluding that the activity in the soil was caused by chemistry or physics. Over the last three decades, investigation of Mars has greatly increased. Soil, rock and atmospheric analyses have been made. Multi-spectral observations have been made from Mars and Earth orbits and from Earth-based telescopes. Knowledge of extreme habitats and bizarre life forms that populate them on Earth has increased dramatically. However, this vast amount of new astrobiological information has yet to be integrated into an objective scientific evaluation of the LR results and the possibilities for life on Mars. Indeed, in part upon misinterpretations of the new findings, myths have been embedded into the scientific literature of Mars. Based on these myths as key ingredients, a false "standard model" of Martian life potential has been developed. It has been accepted by much of the astrobiological community, and, through its endorsement, the world at large. This paper attempts to bring the supportable facts together in calling for a revision of the current consensus regarding life on Mars. It recommends actions to facilitate the paradigm change.

  1. Paleolakes on Mars.

    PubMed

    Wharton, R A; Crosby, J M; McKay, C P; Rice, J W

    1995-01-01

    Observational evidence such as outflow channels and valley networks suggest that in the past there was flowing water on Mars. The images of fluvial features on Mars logically suggest that there must exist downstream locations in which the water pooled and the sediment load deposited (i.e. lakes). Sediments and morphological features associated with the martian paleolakes are believed to occur in Valles Marineris, and several large basins including Amazonis, Chryse and Elysium planitia. As Mars became progressively colder over geological time, any lakes on its surface would have become seasonally, and eventually perennially ice-covered. We know from polar lakes on Earth that ice-covered lakes can persist even when the mean annual temperature falls below freezing. Thus, the most recent lacustrine sediments on Mars were probably deposited in ice-covered lakes. While life outside of the Earth's atmosphere has yet to be observed, there is a general consensus among exobiologists that the search for extraterrestrial life should be based upon liquid water. The inference that there was liquid water on Mars during an earlier epoch is the primary motivation for considering the possibility of life during this time. It would be of enormous interest from both an exobiological and paleolimnological perspective to discover lakes or the evidence of former lakes on another planet such as Mars. Limnology would then become an interplanetary science.

  2. Mars Rover RTG Study

    SciTech Connect

    Schock, Alfred

    1989-11-27

    This report summarizes the results of a Radioisotope Thermoelectric Generator (RTG) design study conducted by Fairchild Space Company at the direction of the U.S. Department of Energy's Office of Special Applications, in support of the Mars Rover and Sample Return mission under investigation at NASA's Jet Propulsion Laboratory. Presented at the 40th Congress of the IAF, Oct. 7-13, 1989 in Torremolinos, Malaga-Spain. The paper describes the design and analysis of Radioisotope Thermoelectric Generators (RTGs) for powering the Mars Rover vehicle, which is a critical element of the unmanned Mars Rover and Sample Return mission (MRSR). The RTG design study was conducted by Fairchild Space for the U.S. DOE in support of the JPL MRSR Project. The paper briefly describes a reference mission scenario, an illustrative Rover design and activity pattern on Mars, and its power system requirements and environmental constraints, including the RTG cooling requirements during transit to Mars. It summarizes the baseline RTG's mass breakdown, and presents a detailed description of its thermal, thermoelectric, and electrical analysis. The results presented show the RTG performance achievable with current technology, and the performance improvements that would be achievable with various technology developments. It provides a basis for selecting the optimum strategy for meeting the Mars Rover design goals with minimal programmatic risk and cost. Cross Reference CID #7135 dated 10/1989. There is a duplicate copy. This document is not relevant to the OSTI Library. Do not send.

  3. Transportation: Destination Mars

    NASA Astrophysics Data System (ADS)

    Eoff, Bill

    1998-01-01

    As the agency space transportation lead center, Marshall Space Flight Center has been conducting transportation assessments for future robotic and human Mars missions to identify critical technologies. Five human Mars options are currently under assessment with each option including all transportation requirements from Earth to Mars and return. The primary difference for each option is the propulsion source from Earth to Mars. In case any of the options require heavy launch capability that is not currently projected as available, an in-house study has been initiated to determine the most cost effective means of providing such launch capability. This assessment is only considering launch architectures that support the overall human Mars mission cost goal of 25B. The guidelines for the launch capability study included delivery of 80 metric ton (176 KLB) payloads, 25 feet diameter x 92 feet long, to 220 nmi orbits at 28.5 degrees. The launch vehicle concept of the study was designated "Magnum" to differentiate from prior heavy launch vehicle assessments. This assessment along with the assessment of options for all transportation phases of a Mars mission are on-going.

  4. Real Time Mars Approach Navigation Aided by the Mars Network

    NASA Technical Reports Server (NTRS)

    Ely, Todd A.; Duncan, Courtney; Lightsey, E. Glenn; Mogensen, Andreas

    2006-01-01

    A NASA Mars technology project is described that is building a prototype embedded real time Mars approach navigation capability which can be hosted on the Mars Network's Electra transceiver. The paper motivates the reason for doing real time Mars approach navigation via a set of analyses demonstrating its utility for enabling Mars pin-point landing (less than 1-km landing error). The development approach, software design, and test results are discussed. Finally, the way forward towards a flight demonstration on the Mars Science Laboratory (MSL) is presented.

  5. Real Time Mars Approach Navigation Aided by the Mars Network

    NASA Technical Reports Server (NTRS)

    Ely, Todd A.; Duncan, Courtney; Lightsey, E. Glenn; Mogensen, Andreas

    2006-01-01

    A NASA Mars technology project is described that is building a prototype embedded real time Mars approach navigation capability which can be hosted on the Mars Network's Electra transceiver. The paper motivates the reason for doing real time Mars approach navigation via a set of analyses demonstrating its utility for enabling Mars pin-point landing (< 1-km landing error). The development approach, software design, and test results are discussed. Finally, the way forward towards a flight demonstration on the Mars Science Laboratory is presented.

  6. Mars at Ls 357o

    NASA Technical Reports Server (NTRS)

    2006-01-01

    31 January 2006 This picture is a composite of Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) daily global images acquired at Ls 357o during a previous Mars year. This month, Mars looks similar, as Ls 357o occurred in mid-January 2006. The picture shows the south polar region of Mars. Over the course of the month, additional faces of Mars as it appears at this time of year are being posted for MOC Picture of the Day. Ls, solar longitude, is a measure of the time of year on Mars. Mars travels 360o around the Sun in 1 Mars year. The year begins at Ls 0o, the start of northern spring and southern autumn.

    Season: Northern Winter/Southern Summer

  7. Mars at Ls 324o

    NASA Technical Reports Server (NTRS)

    2005-01-01

    29 November 2005 This picture is a composite of Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) daily global images acquired at Ls 324o during a previous Mars year. This month, Mars looks similar, as Ls 324o occurred in mid-November 2005. The picture shows the south polar region of Mars. Over the course of the month, additional faces of Mars as it appears at this time of year are being posted for MOC Picture of the Day. Ls, solar longitude, is a measure of the time of year on Mars. Mars travels 360o around the Sun in 1 Mars year. The year begins at Ls 0o, the start of northern spring and southern autumn.

    Season: Northern Winter/Southern Summer

  8. Mars Telecommunications Orbiter, Artist's Concept

    NASA Technical Reports Server (NTRS)

    2005-01-01

    This illustration depicts a concept for NASA's Mars Telecommunications Orbiter in flight around Mars. The orbiter is in development to be the first spacecraft with a primary function of providing communication links while orbiting a foreign planet. The project's plans call for launch in September 2009, arrival at Mars in August 2010 and a mission of six to 10 years while in orbit. Mars Telecommunication Orbiter would serve as the Mars hub for an interplanetery Internet, greatly increasing the information payoff from other future Mars missions. The mission is designed to orbit Mars more than 10 times farther from the planet than orbiters dedicated primarily to science. The high-orbit design minimizes the time that Mars itself blocks the orbiter from communicating with Earth and maximizes the time that the orbiter is above the horizon -- thus capable of communications relay -- for rovers and stationary landers on Mars' surface.

  9. The MARS2013 Mars analog mission.

    PubMed

    Groemer, Gernot; Soucek, Alexander; Frischauf, Norbert; Stumptner, Willibald; Ragonig, Christoph; Sams, Sebastian; Bartenstein, Thomas; Häuplik-Meusburger, Sandra; Petrova, Polina; Evetts, Simon; Sivenesan, Chan; Bothe, Claudia; Boyd, Andrea; Dinkelaker, Aline; Dissertori, Markus; Fasching, David; Fischer, Monika; Föger, Daniel; Foresta, Luca; Fritsch, Lukas; Fuchs, Harald; Gautsch, Christoph; Gerard, Stephan; Goetzloff, Linda; Gołebiowska, Izabella; Gorur, Paavan; Groemer, Gerhard; Groll, Petra; Haider, Christian; Haider, Olivia; Hauth, Eva; Hauth, Stefan; Hettrich, Sebastian; Jais, Wolfgang; Jones, Natalie; Taj-Eddine, Kamal; Karl, Alexander; Kauerhoff, Tilo; Khan, Muhammad Shadab; Kjeldsen, Andreas; Klauck, Jan; Losiak, Anna; Luger, Markus; Luger, Thomas; Luger, Ulrich; McArthur, Jane; Moser, Linda; Neuner, Julia; Orgel, Csilla; Ori, Gian Gabriele; Paternesi, Roberta; Peschier, Jarno; Pfeil, Isabella; Prock, Silvia; Radinger, Josef; Ramirez, Barbara; Ramo, Wissam; Rampey, Mike; Sams, Arnold; Sams, Elisabeth; Sandu, Oana; Sans, Alejandra; Sansone, Petra; Scheer, Daniela; Schildhammer, Daniel; Scornet, Quentin; Sejkora, Nina; Stadler, Andrea; Stummer, Florian; Taraba, Michael; Tlustos, Reinhard; Toferer, Ernst; Turetschek, Thomas; Winter, Egon; Zanella-Kux, Katja

    2014-05-01

    We report on the MARS2013 mission, a 4-week Mars analog field test in the northern Sahara. Nineteen experiments were conducted by a field crew in Morocco under simulated martian surface exploration conditions, supervised by a Mission Support Center in Innsbruck, Austria. A Remote Science Support team analyzed field data in near real time, providing planning input for the management of a complex system of field assets; two advanced space suit simulators, four robotic vehicles, an emergency shelter, and a stationary sensor platform in a realistic work flow were coordinated by a Flight Control Team. A dedicated flight planning group, external control centers for rover tele-operations, and a biomedical monitoring team supported the field operations. A 10 min satellite communication delay and other limitations pertinent to human planetary surface activities were introduced. The fields of research for the experiments were geology, human factors, astrobiology, robotics, tele-science, exploration, and operations research. This paper provides an overview of the geological context and environmental conditions of the test site and the mission architecture, in particular the communication infrastructure emulating the signal travel time between Earth and Mars. We report on the operational work flows and the experiments conducted, including a deployable shelter prototype for multiple-day extravehicular activities and contingency situations.

  10. Examining Mars with SPICE

    NASA Technical Reports Server (NTRS)

    Acton, Charles H.; Bachman, Nathaniel J.; Bytof, Jeff A.; Semenov, Boris V.; Taber, William; Turner, F. Scott; Wright, Edward D.

    1999-01-01

    The International Mars Conference highlights the wealth of scientific data now and soon to be acquired from an international armada of Mars-bound robotic spacecraft. Underlying the planning and interpretation of these scientific observations around and upon Mars are ancillary data and associated software needed to deal with trajectories or locations, instrument pointing, timing and Mars cartographic models. The NASA planetary community has adopted the SPICE system of ancillary data standards and allied tools to fill the need for consistent, reliable access to these basic data and a near limitless range of derived parameters. After substantial rapid growth in its formative years, the SPICE system continues to evolve today to meet new needs and improve ease of use. Adaptations to handle landers and rovers were prototyped on the Mars pathfinder mission and will next be used on Mars '01-'05. Incorporation of new methods to readily handle non-inertial reference frames has vastly extended the capability and simplified many computations. A translation of the SPICE Toolkit software suite to the C language has just been announced. To further support cartographic calculations associated with Mars exploration the SPICE developers at JPL have recently been asked by NASA to work with cartographers to develop standards and allied software for storing and accessing control net and shape model data sets; these will be highly integrated with existing SPICE components. NASA specifically supports the widest possible utilization of SPICE capabilities throughout the international space science community. With NASA backing the Russian Space Agency and Russian Academy of Science adopted the SPICE standards for the Mars 96 mission. The SPICE ephemeris component will shortly become the international standard for agencies using the Deep Space Network. U.S. and European scientists hope that ESA will employ SPICE standards on the Mars Express mission. SPICE is an open set of standards, and

  11. Comparison of polyglactin-910 and polydioxanone for closure of the linea alba following caudal ventral midline laparotomy in sheep

    PubMed Central

    Rousseau, Marjolaine; Anderson, David E.; Rozell, Timothy G.; Hand, Jacqelyn M.; Faris, Brian R.

    2015-01-01

    This study compared incisional complications after ventral midline laparotomy using 2 absorbable suture materials for apposition of the linea alba in sheep. The linea alba of 93 yearling sheep was sutured by 3 veterinarians in a simple continuous pattern using either polyglactin 910 (PG910; group PG) or polydioxanone (PDS; group PD). A blinded observer assessed surgical sites at the time of suture removal. Multivariate logistic regression was used to assess the association between incisional complications and variables (suture material used, veterinarian, skin suture removal time). The odds of incisional complications did not vary significantly with the type of suture material used (P = 0.11), veterinarian (P = 0.61) or skin suture removal time (P = 0.36). Most incisional complications were cutaneous suture sinus formation. Either PG910 or PDS may be used for linea alba closure in sheep. PMID:26345301

  12. Annotation and re-sequencing of genes from de novo transcriptome assembly of Abies alba (Pinaceae)1

    PubMed Central

    Roschanski, Anna M.; Fady, Bruno; Ziegenhagen, Birgit; Liepelt, Sascha

    2013-01-01

    • Premise of the study: We present a protocol for the annotation of transcriptome sequence data and the identification of candidate genes therein using the example of the nonmodel conifer Abies alba. • Methods and Results: A normalized cDNA library was built from an A. alba seedling. The sequencing on a 454 platform yielded more than 1.5 million reads that were de novo assembled into 25149 contigs. Two complementary approaches were applied to annotate gene fragments that code for (1) well-known proteins and (2) proteins that are potentially adaptively relevant. Primer development and testing yielded 88 amplicons that could successfully be resequenced from genomic DNA. • Conclusions: The annotation workflow offers an efficient way to identify potential adaptively relevant genes from the large quantity of transcriptome sequence data. The primer set presented should be prioritized for single-nucleotide polymorphism detection in adaptively relevant genes in A. alba. PMID:25202477

  13. Comparison of polyglactin-910 and polydioxanone for closure of the linea alba following caudal ventral midline laparotomy in sheep.

    PubMed

    Rousseau, Marjolaine; Anderson, David E; Rozell, Timothy G; Hand, Jacqelyn M; Faris, Brian R

    2015-09-01

    This study compared incisional complications after ventral midline laparotomy using 2 absorbable suture materials for apposition of the linea alba in sheep. The linea alba of 93 yearling sheep was sutured by 3 veterinarians in a simple continuous pattern using either polyglactin 910 (PG910; group PG) or polydioxanone (PDS; group PD). A blinded observer assessed surgical sites at the time of suture removal. Multivariate logistic regression was used to assess the association between incisional complications and variables (suture material used, veterinarian, skin suture removal time). The odds of incisional complications did not vary significantly with the type of suture material used (P = 0.11), veterinarian (P = 0.61) or skin suture removal time (P = 0.36). Most incisional complications were cutaneous suture sinus formation. Either PG910 or PDS may be used for linea alba closure in sheep.

  14. Mars Odyssey Seen by Mars Global Surveyor (3-D)

    NASA Technical Reports Server (NTRS)

    2005-01-01

    This stereoscopic picture of NASA's Mars Odyssey spacecraft was created from two views of that spacecraft taken by the Mars Orbiter Camera on NASA's Mars Global Surveyor. The camera's successful imaging of Odyssey and of the European Space Agency's Mars Express in April 2005 produced the first pictures of any spacecraft orbiting Mars taken by another spacecraft orbiting Mars.

    Mars Global Surveyor acquired this image of Mars Odyssey on April 21, 2005. The stereoscopic picture combines one view captured while the two orbiters were 90 kilometers (56 miles) apart with a second view captured from a slightly different angle when the two orbiters were 135 kilometers (84 miles) apart. For proper viewing, the user needs '3-D' glasses with red over the left eye and blue over the right eye.

    The Mars Orbiter Camera can resolve features on the surface of Mars as small as a few meters or yards across from Mars Global Surveyor's orbital altitude of 350 to 405 kilometers (217 to 252 miles). From a distance of 100 kilometers (62 miles), the camera would be able to resolve features substantially smaller than 1 meter or yard across.

    Mars Odyssey was launched on April 7, 2001, and reached Mars on Oct. 24, 2001. Mars Global Surveyor left Earth on Nov. 7, 1996, and arrived in Mars orbit on Sept. 12, 1997. Both orbiters are in an extended mission phase, both have relayed data from the Mars Exploration Rovers, and both are continuing to return exciting new results from Mars. JPL, a division of the California Institute of Technology, Pasadena, manages both missions for NASA's Science Mission Directorate, Washington, D.C.

  15. Uncorrected land-use planning highlighted by flooding: the Alba case study (Piedmont, Italy)

    NASA Astrophysics Data System (ADS)

    Luino, F.; Turconi, L.; Petrea, C.; Nigrelli, G.

    2012-07-01

    Alba is a town of over 30 000 inhabitants located along the Tanaro River (Piedmont, northwestern Italy) and is famous for its wine and white truffles. Many important industries and companies are based in Alba, including the famous confectionery group Ferrero. The town suffered considerably from a flood that occurred on 5-6 November 1994. Forty-eight percent of the urban area was inundated, causing severe damage and killing nine people. After the flood, the Alba area was analysed in detail to determine the reasons for its vulnerability. Information on serious floods in this area since 1800 was gathered from official records, state technical office reports, unpublished documents in the municipal archives, and articles published in local and national newspapers. Maps, plans and aerial photographs (since 1954) were examined to reconstruct Alba's urban development over the last two centuries and the planform changes of the Tanaro River. The results were compared with the effects of the November 1994 flood, which was mapped from aerial photographs taken immediately after the flood, field surveys and eyewitness reports. The territory of Alba was subdivided into six categories: residential; public service; industrial, commercial and hotels; sports areas, utilities and standards (public gardens, parks, athletics grounds, private and public sport clubs); aggregate plants and dumps; and agriculture and riverine strip. The six categories were then grouped into three classes with different flooding-vulnerability levels according to various parameters. Using GIS, the three river corridors along the Tanaro identified by the Autorità di Bacino del Fiume Po were overlaid on the three classes to produce a final map of the risk areas. This study shows that the historic floods and their dynamics have not been duly considered in the land-use planning of Alba. The zones that were most heavily damaged in the 1994 flood were those that were frequently affected in the past and sites of

  16. The case for Mars II

    NASA Technical Reports Server (NTRS)

    Mckay, C. P. (Editor)

    1985-01-01

    Among the topics discussed are: the political aspects of the exploration of Mars, preparatory mission scenarios in advance of manned Martian exploration, and scientific programs for a base on Mars. Consideration is also given to: mission strategies and spacecraft design for a Mars base program; concepts for the realization of a manned mission to Mars; dirigible airship applications to Martian surface exploration; and the power requirements of several Martian base designs. Additional topics include: the impact of propellant manufacturing on early manned exploration of the solar system; water supply issues for a manned Mars base; and psychological and interpersonal adaptation to life on Mars.

  17. Preventive effects of Morus alba L. anthocyanins on diabetes in Zucker diabetic fatty rats

    PubMed Central

    SARIKAPHUTI, ARIYA; NARARATWANCHAI, THAMTHIWAT; HASHIGUCHI, TERUTO; ITO, TAKASHI; THAWORANUNTA, SITA; KIKUCHI, KIYOSHI; OYAMA, YOKO; MARUYAMA, IKURO; TANCHAROEN, SALUNYA

    2013-01-01

    The mulberry plant (Morus alba L.) contains abundant anthocyanins (ANCs), which are natural antioxidants. The aim of this study was to determine the ANC composition of Thai Morus alba L. fruits and to assess the effect of an ANC extract on blood glucose and insulin levels in male leptin receptor-deficient Zucker diabetic fatty (ZDF) rats. The major components of the ANC extract were identified by high-performance liquid chromatography-electrospray ionization-mass spectrometry. ZDF and lean rats were treated with 125 or 250 mg ANCs/kg body weight, or 1% carboxymethylcellulose (CMC) twice daily for 5 weeks. Neither ANC dose had an effect on body weight. Following 5 weeks of treatment, glucose levels were observed to increase from 105.5±8.7 to 396.25±21 mg/dl (P<0.0001) in the CMC-treated ZDF rats; however, the glucose levels were significantly lower in the rats treated with 125 or 250 mg/kg ANCs (228.25±45 and 131.75±10 mg/dl, respectively; P<0.001 versus CMC). The administration of 250 mg/kg ANCs normalized glucose levels in the ZDF rats towards those of the lean littermates. Insulin levels were decreased significantly in the ZDF rats treated with CMC or 125 mg/kg ANCs (P<0.0001), but not in the rats treated with 250 mg/kg ANCs. Histologically, 250 mg/kg ANCs was observed to prevent islet degeneration compared with the islets in CMC-treated rats. This study, demonstrated that ANCs extracted from Morus alba L. were well tolerated and exhibited effective anti-diabetic properties in ZDF rats. ANCs represent a promising class of therapeutic compounds that may be useful in the prevention of type 2 diabetes. PMID:24137248

  18. Growth of Populus alba and its influence on soil trace element availability.

    PubMed

    Ciadamidaro, L; Madejón, E; Puschenreiter, M; Madejón, P

    2013-06-01

    The use of fast growing trees is a common practice for phytoremediation of contaminated soils. Plant roots can change trace element bioavailability in soils. We studied the effect of Populus alba on trace element bioavailability on two contaminated soils (one with neutral pH and other with acid pH) comparing two methods (0.01 M CaCl2-extractable in soil and concentration in soil pore water SPW), trace element accumulation in leaves and plant development over 36 months. Results were compared to those obtained with a non-contaminated soil. The experiment was carried out in containers (95 L of volume and 1m height). Half of the containers for each soil were planted with P. alba saplings and the others remained without plant. In neutral soils plant growth did not influence soil pH; the greatest effect due to plant growth was found in acid soil. Values of pH obtained by SPW showed a similar trend compared to those obtained after soil KCl extraction. Bioavailability of trace elements determined by both methods followed the same behavior in the three studied soils. Both methods for determining trace element bioavailability in soil were accurate to predict plant uptake. In non-contaminated soil, plants tended to increase micronutrients (Cu, Mn and Zn) availability. However, in case of contaminated soil, the growth of P. alba did not increase trace element availability. Moreover, results on height and diameter of the trunk of the trees, during 36 months, demonstrated that the presence of total trace elements in soil did not affect plant development.

  19. Involvement of an RNA binding protein containing Alba domain in the stage-specific regulation of beta-amastin expression in Trypanosoma cruzi.

    PubMed

    Pérez-Díaz, Leticia; Silva, Tais Caroline; Teixeira, Santuza M R

    2017-01-01

    Amastins are surface glycoproteins, first identified in amastigotes of T. cruzi but later found to be expressed in several Leishmania species, as well as in T. cruzi epimastigotes. Amastins are encoded by a diverse gene family that can be grouped into four subfamilies named α, β, γ, and δ amastins. Differential expression of amastin genes results from regulatory mechanisms involving changes in mRNA stability and/or translational control. Although distinct regulatory elements were identified in the 3' UTR of T. cruzi and Leishmania amastin mRNAs, RNA binding proteins involved with amastin gene regulation have only being characterized in L. infantum where an Alba-domain protein (LiAlba20) able to bind to the 3' UTR of a δ-amastin mRNA was identified. Here we investigated the role of TcAlba30, the LiAlba20 homologue in T. cruzi, in the post transcriptional regulation of amastin genes. TcAlba30 transcripts are present in all stages of the T. cruzi life cycle. RNA immunoprecipitation assays using a transfected cell line expressing a cMyc tagged TcAlba30 revealed that TcAlba30 can interact with β-amastin mRNA. In addition, over-expression of TcAlba30 in epimastigotes resulted in 50% decreased levels of β-amastin mRNAs compared to wild type parasites. Since luciferase assays indicated the presence of regulatory elements in the 3' UTR of β-amastin mRNA and reduced levels of luciferase mRNA were found in parasites over expressing TcAlba30, we conclude that TcAlba30 acts as a T. cruzi RNA binding protein involved in the negative control of β-amastin expression through interactions with its 3'UTR.

  20. Telecommunications systems evolution for Mars Exploration

    NASA Technical Reports Server (NTRS)

    Noreen, Gary; De Paula, Ramon P.; Edwards, Charles D. Jr; Komarek, Thomas; Edwards, Bernard L.; Edwards, Bernard L.; Kerridge, Stuart J.; Diehl, Roger; Franklin, Stephen F.

    2003-01-01

    This paper describes the evolution of telecommunication systems at Mars. It reviews the telecommunications capabilities, technology and limiting factors of current and planned Mars orbiters from Mars Global Surveyor to the planned Mars Telecommunications Orbiter (MTO).

  1. De novo Transcriptome Analysis of Sinapis alba in Revealing the Glucosinolate and Phytochelatin Pathways

    PubMed Central

    Zhang, Xiaohui; Liu, Tongjin; Duan, Mengmeng; Song, Jiangping; Li, Xixiang

    2016-01-01

    Sinapis alba is an important condiment crop and can also be used as a phytoremediation plant. Though it has important economic and agronomic values, sequence data, and the genetic tools are still rare in this plant. In the present study, a de novo transcriptome based on the transcriptions of leaves, stems, and roots was assembled for S. alba for the first time. The transcriptome contains 47,972 unigenes with a mean length of 1185 nt and an N50 of 1672 nt. Among these unigenes, 46,535 (97%) unigenes were annotated by at least one of the following databases: NCBI non-redundant (Nr), Swiss-Prot, Kyoto Encyclopedia of Genes and Genomes (KEGG) pathway, Gene Ontology (GO), and Clusters of Orthologous Groups of proteins (COGs). The tissue expression pattern profiles revealed that 3489, 1361, and 8482 unigenes were predominantly expressed in the leaves, stems, and roots of S. alba, respectively. Genes predominantly expressed in the leaf were enriched in photosynthesis- and carbon fixation-related pathways. Genes predominantly expressed in the stem were enriched in not only pathways related to sugar, ether lipid, and amino acid metabolisms but also plant hormone signal transduction and circadian rhythm pathways, while the root-dominant genes were enriched in pathways related to lignin and cellulose syntheses, involved in plant-pathogen interactions, and potentially responsible for heavy metal chelating, and detoxification. Based on this transcriptome, 14,727 simple sequence repeats (SSRs) were identified, and 12,830 pairs of primers were developed for 2522 SSR-containing unigenes. Additionally, the glucosinolate (GSL) and phytochelatin metabolic pathways, which give the characteristic flavor and the heavy metal tolerance of this plant, were intensively analyzed. The genes of aliphatic GSLs pathway were predominantly expressed in roots. The absence of aliphatic GSLs in leaf tissues was due to the shutdown of BCAT4, MAM1, and CYP79F1 expressions. Glutathione was extensively

  2. Six new record species of whiteflies (Hemiptera: Aleyrodidae) infesting Morus alba in China.

    PubMed

    Wang, Ji-Rui; Song, Zao-Qin; Du, Yu-Zhou

    2014-01-01

    To determine the species of whiteflies occurring on mulberry, Morus alba L. (Rosales: Moraceae) in China, we collected samples in more than 87 sites in 16 provinces of China from 2008 to 2011. In total, 10 species, representing seven genera of the subfamily Aleyrodinae, were identified. Of these, six species are newly recorded on mulberry in China, namely, Aleuroclava ficicola Takahashi, Aleuroclava gordoniae (Takahashi), Aleurotrachelus camelliae (Kuwana), Bemisia afer (Priesner & Hosny), Bemisia tabaci Gennadius, and Pealius machili Takahashi. Information on the taxonomy, distribution, and host plants of the whitefly species found on mulberry in China, along with a brief description and illustrations of each species are provided.

  3. Human colon cancer HT-29 cell death responses to doxorubicin and Morus Alba leaves flavonoid extract.

    PubMed

    Fallah, S; Karimi, A; Panahi, G; Gerayesh Nejad, S; Fadaei, R; Seifi, M

    2016-03-31

    The mechanistic basis for the biological properties of Morus alba flavonoid extract (MFE) and chemotherapy drug of doxorubicin on human colon cancer HT-29 cell line death are unknown. The effect of doxorubicin and flavonoid extract on colon cancer HT-29 cell line death and identification of APC gene expression and PARP concentration of HT-29 cell line were investigated. The results showed that flavonoid extract and doxorubicin induce a dose dependent cell death in HT-29 cell line. MFE and doxorubicin exert a cytotoxic effect on human colon cancer HT-29 cell line by probably promoting or induction of apoptosis.

  4. Pityriasis Alba--Common Disease, Enigmatic Entity: Up-to-Date Review of the Literature.

    PubMed

    Miazek, Nina; Michalek, Irmina; Pawlowska-Kisiel, Malgorzata; Olszewska, Malgorzata; Rudnicka, Lidia

    2015-01-01

    Pityriasis alba (PA) is a skin disorder that affects children and adolescents. Although it is common worldwide, its incidence is markedly higher in darker skin phototypes. Its characteristic features include an extended, multistage course and spontaneous remissions and recurrences. Preceded by erythematous changes, patches of hypopigmented skin of up to a few centimeters in diameter appear on the upper body. Pruritus may accompany it. Even though its etiology is unknown, possible reported triggering factors include sunlight, beauty treatments, and microorganisms, among others. Calcineurin inhibitors play the most crucial role in PA pharmacotherapy. PA often coexists with atopic dermatitis and is considered one of its milder forms.

  5. Simulating "Mars on Earth"

    NASA Technical Reports Server (NTRS)

    Clancey, William J.; Clancy, Daniel (Technical Monitor)

    2002-01-01

    By now, everyone who's heard of the Haughton-Mars Project knows that we travel to Devon Island to learn how people will live and work on Mars. But how do we learn about Mars operations from what happens in the Arctic? We must document our experience--traverses, life in the hab, instrument deployment, communications, and so on. Then we must analyze and formally model what happens. In short, while most scientists are studying the crater, other scientists must be studying the expedition itself. That's what I have done in the past four field seasons. I study field science, both as it naturally occurs at Haughton (unconstrained by a "Mars Sam") and as a constrained experiment using the Flashline Mars Arctic Research Station. During the second week of July 2001, I lived and worked in the hab as part of the Phase 2 crew of six. Besides participating in all activities, I took many photographs and time lapse video. The result of my work will be a computer simulation of how we lived and worked in the hab. It won't be a model of particular people or even my own phase per se, but a pastiche that demonstrates (a proof of concept) that we have appropriate tools for simulating the layout of the hab and daily routines followed by the group and individual scientists. Activities-how people spend their time-are the focus of my observations for building such a simulation model.

  6. The Mars Technology Program

    NASA Technical Reports Server (NTRS)

    Hayati, Samad A.

    2002-01-01

    Future Mars missions require new capabilities that currently are not available. The Mars Technology Program (MTP) is an integral part of the Mars Exploration Program (MEP). Its sole purpose is to assure that required technologies are developed in time to enable the baselined and future missions. The MTP is a NASA-wide technology development program managed by JPL. It is divided into a Focused Program and a Base Program. The Focused Program is tightly tied to the proposed Mars Program mission milestones. It involves time-critical deliverables that must be developed in time for infusion into the proposed Mars 2005, and, 2009 missions. In addition a technology demonstration mission by AFRL will test a LIDAR as part of a joint NASNAFRL experiment. This program bridges the gap between technology and projects by vertically integrating the technology work with pre-project development in a project-like environment with critical dates for technology infusion. A Base Technology Program attacks higher riskhigher payoff technologies not in the critical path of missions.

  7. Mars digital terrain model

    NASA Technical Reports Server (NTRS)

    Wu, Sherman S. C.; Howington, Annie-Elpis

    1987-01-01

    The Mars Digital Terrain Model (DTM) is the result of a new project to: (1) digitize the series of 1:2,000,000-scale topographic maps of Mars, which are being derived photogrammetically under a separate project, and (2) reformat the digital contour information into rasters of elevation that can be readily registered with the Digital Image Model (DIM) of Mars. Derivation of DTM's involves interpolation of elevation values into 1/64-degree resolution and transformation of them to a sinusoidal equal-area projection. Digital data are produced in blocks corresponding with the coordinates of the original 1:2,000,000-scale maps, i.e., the dimensions of each block in the equatorial belt are 22.5 deg of longitude and 15 deg of latitude. This DTM is not only compatible with the DIM, but it can also be registered with other data such as geologic units or gravity. It will be the most comprehensive record of topographic information yet compiled for the Martian surface. Once the DTM's are established, any enhancement of Mars topographic information made with updated data, such as data from the planned Mars Observer Mission, will be by mathematical transformation of the DTM's, eliminating the need for recompilation.

  8. Mars Climate Orbiter

    NASA Technical Reports Server (NTRS)

    1998-01-01

    The Mars Surveyor '98 Climate Orbiter is shown here during acoustic tests that simulate launch conditions. The orbiter was to conduct a two year primary mission to profile the Martian atmosphere and map the surface. To carry out these scientific objectives, the spacecraft carried a rebuilt version of the pressure modulated infrared radiometer, lost with the Mars Observer spacecraft, and a miniaturized dual camera system the size of a pair of binoculars, provided by Malin Space Science Systems, Inc., San Diego, California. During its primary mission, the orbiter was to monitor Mars atmosphere and surface globally on a daily basis for one Martian year (two Earth years), observing the appearance and movement of atmospheric dust and water vapor, as well as characterizing seasonal changes of the planet's surface. Imaging of the surface morphology would also provide important clues about the planet's climate in its early history. The mission was part of NASA's Mars Surveyor program, a sustained program of robotic exploration of the red planet, managed by the Jet Propulsion Laboratory for NASA's Office of Space Science, Washington, DC. Lockheed Martin Astronautics was NASA's industrial partner in the mission. Unfortunately, Mars Climate Orbiter burned up in the Martian atmosphere on September 23, 1999, due to a metric conversion error that caused the spacecraft to be off course.

  9. Phoenix's Position on Mars

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on the image for the animation

    This animation shows an orbital view sweeping upward from Olympus Mons, the tallest volcano in the solar system, to the location of NASA's Phoenix Mars Lander in the northern polar reaches of Mars. The animation then zooms in on the flat terrain where Phoenix touched down May 25, 2008.

    Phoenix eased down to the surface of Mars at approximately 68 degrees north latitude, 234 degrees east longitude, landing in the center of the red circle at the end of the animation. Before Phoenix landed, engineers had predicted it would land within the blue ellipse.

    Phoenix touched down on the Red Planet at 4:53 p.m. Pacific Time (7:53 p.m. Eastern Time), May 25, 2008, in an arctic region called Vastitas Borealis.

    The shaded relief map is based on data from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor orbiter.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  10. Mars Rover RTG Study

    SciTech Connect

    Schock, Alfred

    1989-10-01

    Presented at the 40th Congress of the IAF, Oct. 7-13, 1989 in Torremolinos, Malaga-Spain. The paper describes the design and analysis of Radioisotope Thermoelectric Generators (RTGs) for powering the Mars Rover vehicle, which is a critical element of the unmanned Mars Rover and Sample Return mission (MRSR). The RTG design study was conducted by Fairchild Space for the U.S. DOE in support of the JPL MRSR Project. The paper briefly describes a reference mission scenario, an illustrative Rover design and activity pattern on Mars, and its power system requirements and environmental constraints, including the RTG cooling requirements during transit to Mars. It summarizes the baseline RTG's mass breakdown, and presents a detailed description of its thermal, thermoelectric, and electrical analysis. The results presented show the RTG performance achievable with current technology, and the performance improvements that would be achievable with various technology developments. It provides a basis for selecting the optimum strategy for meeting the Mars Rover design goals with minimal programmatic risk and cost. There is a duplicate copy and three copies in the file.

  11. Journey of a Lifetime -- Mars

    NASA Video Gallery

    NASA wants you to be part of the Journey to Mars. Today, NASA is pushing the boundaries of technology and innovation. NASA’s fleet of robotic scientific explorers at Mars are paving the way for hu...

  12. Mars penetrator: Subsurface science mission

    NASA Technical Reports Server (NTRS)

    Lumpkin, C. K.

    1974-01-01

    A penetrator system to emplace subsurface science on the planet Mars is described. The need for subsurface science is discussed, and the technologies for achieving successful atmospheric entry, Mars penetration, and data retrieval are presented.

  13. Mars ultraviolet simulation facility.

    PubMed

    Zill, L P; Mack, R; DeVincenzi, D L

    1979-12-01

    A facility was established for long-duration ultraviolet (UV) radiation exposure of natural and synthetic materials in order to test hypotheses concerning Martian soil chemistry observed by the Viking Mars landers. The system utilized a 2500 watt xenon lamp as the radiation source, with the beam passing through a heat-dissipating water filter before impinging upon an exposure chamber containing the samples to be irradiated. The chamber was designed to allow for continuous tumbling of the samples, maintenance of temperatures below 0 degrees C during exposure, and monitoring of beam intensity. The facility also provided for sample preparation under a variety of atmospheric conditions, in addition to the Mars nominal. As many as 33 sealed sample ampules have been irradiated in a single exposure. Over 100 samples have been irradiated for approximately 100 to 700 h. The facility has performed well in providing continuous UV irradiation of multiple samples for long periods of time under simulated Mars atmospheric and thermal conditions.

  14. Mars Spark Source Prototype

    NASA Technical Reports Server (NTRS)

    Eichenberg, Dennis J.; Lindamood, Glenn R.; Weiland, Karen J.; VanderWal, Randall L.

    1999-01-01

    The Mars Spark Source Prototype (MSSP) hardware has been developed as part of a proof of concept system for the detection of trace metals such as lead, cadmium, and arsenic in Martian dusts and soils. A spark discharge produces plasma from a soil sample and detectors measure the optical emission from metals in the plasma that will allow their identification and quantification. Trace metal measurements are vital for the assessment of the potential toxicity of the Martian environment for human exploration. The current method of X-ray fluorescence can yield concentrations only of major species. Other instruments are incompatible with the volume, weight, and power constraints for a Mars mission. The instrument will be developed primarily for use in the Martian environment, but would be adaptable for terrestrial use in environmental monitoring. This paper describes the Mars Spark Source Prototype hardware, the results of the characterization tests, and future plans for hardware development.

  15. Mars transportation system

    NASA Technical Reports Server (NTRS)

    Garrard, William; Vano, Andrew; Rutherford, Dave

    1992-01-01

    The University of Minnesota Advanced Space Design Program has developed a sample Mars exploration scenario. The purpose of the design project is to enhance NASA and university interaction, to provide fresh ideas to NASA, and to provide real world design problems to engineering students. The Mars Transportation System in this paper is designed to transport a crew of six astronauts to the Martian surface and return them to Low Earth Orbit (LEO) starting in the year 2016. The proposed vehicle features such advanced technologies as nuclear propulsion, nuclear power generation, and aerobraking. Three missions are planned. Orbital trajectories are of the conjunction class with an inbound Venus swingby providing a 60-day surface stay at Mars and an average total trip time of 520 days.

  16. Spiders from Mars?

    NASA Technical Reports Server (NTRS)

    2003-01-01

    MGS MOC Release No. MOC2-426, 19 July 2003

    No, this is not a picture of a giant, martian spider web. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a plethora of polygonal features on the floor of a northern hemisphere impact crater near 65.6oN, 327.7oW. The picture was acquired during spring, after the seasonal carbon dioxide frost cap had largely migrated through the region. At the time the picture was taken, remnants of seasonal frost remained on the crater rim and on the edges of the troughs that bound each of the polygons. Frost often provides a helpful hint as to where polygons and patterned ground occur. The polygons, if they were on Earth, would indicate the presence of freeze-thaw cycles in ground ice. Although uncertain, the same might be true of Mars. Sunlight illuminates the scene from the lower left.

  17. Remanent magnetism at Mars

    NASA Technical Reports Server (NTRS)

    Curtis, S. A.; Ness, N. F.

    1988-01-01

    It is shown that a strong case can be made for an intrinsic magnetic field of dynamo origin for Mars earlier in its history. The typical equatorial magnetic field intensity would have been equal to about 0.01-0.1 gauss. The earlier dynamo activity is no longer extant, but a significant remanent magnetic field may exist. A highly non-dipole magnetic field could result from the remanent magnetization of the surface. Remanent magnetization may thus play an important role in the Mars solar wind interactions, in contrast to Venus with its surface temperatures above the Curie point. The anomalous characteristics of Mars'solar wind interaction compared to that of Venus may be explicable on this basis.

  18. The channels of Mars

    NASA Technical Reports Server (NTRS)

    Baker, V. R.

    1982-01-01

    Early observations of Mars conducted by means of telescopes are considered. Secchi introduced the Italian word 'canale' ('channel') in 1869 to describe apparent lines on the planet's surface. Between 1877 and 1888 Schiaparelli mapped a profusion of 'canali'. Schiaparelli's work led to famous controversies about Mars. This book attempts to investigate the puzzle posed by the Martian channels, taking into account also the results of the studies conducted with the aid of the two orbiting Viking spacecraft which have produced a total number of nearly 60,000 pictures. The channel types are discussed along with questions regarding the distribution, the ages, and the proposed origins of the channels. Attention is given to the geomorphology of Mars, the patterns and networks of Martian valleys, ice and the Martian surface, the outflow channels, catastrophic flood processes, questions of analogy between terrestrial and Martian geographic features, and Martian phenomena associated with water liquid or water ice.

  19. Northern Plains of Mars

    NASA Technical Reports Server (NTRS)

    2004-01-01

    22 November 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a typical view of the martian northern plains. Thousands of square kilometers of the northern middle and polar latitudes of Mars look similar to the scene in this image. In late spring and in summer, dust devils crisscross the northern plains, leaving a variety of dark streaks. The streaks do not survive from year to year, indicating their ephemeral nature. The circular features in this image, including the prominent bright circular feature near the bottom, are the locations of buried meteor impact craters. This image is located near 58.1oN, 207.6oW, and covers an area approximately 3 km (1.9 mi) wide. Sunlight illuminates the scene from the lower left.

  20. Dynamics of Mars' magnetosphere

    SciTech Connect

    Kennel, C.F.; Coroniti, F.V. ); Zelenyi, L.M. ); Moses, S.L.

    1989-08-01

    If Mars has a small intrinsic magnetic moment, Mars' magnetosphere could vary on time scales of a few minutes due to reconnection with the solar wind magnetic field. The day-side magnetopause will be one or two reflected-ion Larmor radii from the bow shock. Substorms will have scale-times of about six minutes. Mars' high ionospheric conductance will virtually stop polar cap convection, and create a magnetic topological crisis unless convecting magnetic flux finds a dissipative way to return to the day-side. The strong magnetic hear induced by magnetospheric convection above the ionosphere could be tearing unstable. The magnetic field might diffusively percolate through the tearing layer. This shearing also draws field aligned currents from the ionosphere which could inject few KeV heavy ionospheric ions into the magnetotail.

  1. The atmosphere of Mars

    NASA Technical Reports Server (NTRS)

    Barth, C. A.

    1974-01-01

    The atmosphere of Mars is essentially a pure carbon dioxide atmosphere that contains a small and seasonably varying amount of water vapor. A number of minor constituents which arise from the interactions of solar radiation with water vapor and carbon dioxide include carbon monoxide, atomic oxygen, molecular oxygen, ozone, and atomic hydrogen. At the surface of Mars the atmospheric pressure is less than one hundredth of the pressure at the surface of the earth. Extensive cloud systems appear on Mars. The structure of the lower Martian atmosphere is discussed together with variations in the lower atmosphere and the characteristics of the upper atmosphere. Reactions of photochemistry are considered along with the atmospheric escape and interactions between the atmosphere and the polar caps.

  2. Climatic change on Mars.

    PubMed

    Sagan, C; Toon, O B; Gierasch, P J

    1973-09-14

    The equatorial sinuous channels on Mars detected by Mariner 9 point to a past epoch of higher pressures and abundant liquid water. Advective instability of the martian atmosphere permits two stable climates-one close to present conditions, the other at a pressure of the order of 1 bar depending on the quantity of buried volatiles. Variations in the obliquity of Mars, the luminosity of the sun, and the albedo of the polar caps each appear capable of driving the instability between a current ice age and more clement conditions. Obliquity driving alone implies that epochs of much higher and of much lower pressure must have characterized martian history. Climatic change on Mars may have important meteorological, geological, and biological implications.

  3. Mars Umbilical Technology Demonstrator

    NASA Technical Reports Server (NTRS)

    Houshangi, Nasser

    2000-01-01

    The objective of this project is to develop a autonomous umbilical mating for the mars umbilical technology demonstrator. The Mars Umbilical Technology Demonstrator (MUTD) shall provide electrical power and fiber optic data cable connections between two simulated mars vehicles. The Omnibot is used to provide the mobile base for the system. The mate to umbilical plate is mounted on a three axis Cartesian table, which is installed on the Omnibot mobile base. The Omnibot is controlled in a teleoperated mode. The operator using the vision system will guide the Omnibot to get close to the mate to plate. The information received from four ultrasonic sensors is used to identify the position of mate to plate and mate the umbilical plates autonomously. A successful experimentation verifies the approach.

  4. The Mars Pathfinder Mission

    NASA Astrophysics Data System (ADS)

    Golombek, M. P.

    1996-09-01

    The Mars Pathfinder mission is a Discovery class mission that will place a small lander and rover on the surface of Mars on July 4, 1997. The Pathfinder flight system is a single small lander, packaged within an aeroshell and back cover with a back-pack-style cruise stage. The vehicle will be launched, fly independently to Mars, and enter the atmosphere directly on approach behind the aeroshell. The vehicle is slowed by a parachute and 3 small solid rockets before landing on inflated airbags. Petals of a small tetrahedron shaped lander open up, to right the vehicle. The lander is solar powered with batteries and will operate on the surface for up to a year, downlinking data on a high-gain antenna. Pathfinder will be the first mission to use a rover, with 3 imagers and an alpha proton X-ray spectrometer, to characterize the rocks and soils in a landing area over hundreds of square meters on Mars, which will provide a calibration point or "ground truth" for orbital remote sensing observations. The rover (includes a series of technology experiments), the instruments (including a stereo multispectral surface imager on a pop up mast and an atmospheric structure instrument-surface meteorology package) and the telemetry system will allow investigations of: the surface morphology and geology at meter scale, the petrology and geochemistry of rocks and soils, the magnetic properties of dust, soil mechanics and properties, a variety of atmospheric investigations and the rotational and orbital dynamics of Mars. Landing downstream from the mouth of a giant catastrophic outflow channel, Ares Vallis, offers the potential of identifying and analyzing a wide variety of crustal materials, from the ancient heavily cratered terrain, intermediate-aged ridged plains and reworked channel deposits, thus allowing first-order scientific investigations of the early differentiation and evolution of the crust, the development of weathering products and early environments and conditions on Mars.

  5. Meteorites on Mars

    NASA Technical Reports Server (NTRS)

    Flynn, G. J.; Mckay, D. S.

    1988-01-01

    Four types of meteoritic material should be found on Mars: (1) micrometeorites, many of which will survive atmospheric entry unmelted, which should fall relatively uniformly over the planet's surface, (2) ablation products from larger meteorites which ablate, break up and burn up in the Mars atmosphere, (3) debris from large, crater forming objects, which, by analogy to terrestrial and lunar impact events, will be concentrated in the crater ejecta blankets (except for rare, large events, such as the proposed C-T event on earth, which can distribute debris on a planetary scale), and (4) debris from the early, intense bombardment, which, in many areas of the planet, may now be incorporated into rocks by geologic processes subsequent to the intense bombardment era. To estimate the extent of meteoritic addition to indigenous Martian material, the meteoritic flux on Mars must be known. It is estimated that the overall flux is twice that for the Moon and 1.33 that for Earth. For small particles, whose orbital evolution is dominated by Poynting Robertson drag, the flux at Mars can be estimated from the Earth flux. The smaller Martian gravitational enhancement as well as the decrease in the spatial density of interplanetary dust with increasing heliocentric distance should reduce the flux of small particles at Mars to about 0.33 times the flux at Earth. Because of the smaller planetary cross-section the total infalling mass at Mars is then estimated to be 0.09 time the infalling mass in the micrometeorite size range at Earth.

  6. PERCIVAL mission to Mars

    NASA Technical Reports Server (NTRS)

    Reed, David W.; Lilley, Stewart; Sirman, Melinda; Bolton, Paul; Elliott, Susan; Hamilton, Doug; Nickelson, James; Shelton, Artemus

    1992-01-01

    With the downturn of the world economy, the priority of unmanned exploration of the solar system has been lowered. Instead of foregoing all missions to our neighbors in the solar system, a new philosophy of exploration mission design has evolved to insure the continued exploration of the solar system. The 'Discovery-class' design philosophy uses a low cost, limited mission, available technology spacecraft instead of the previous 'Voyager-class' design philosophy that uses a 'do-everything at any cost' spacecraft. The Percival Mission to Mars was proposed by Ares Industries as one of the new 'Discovery-class' of exploration missions. The spacecraft will be christened Percival in honor of American astronomer Percival Lowell who proposed the existence of life on Mars in the early twentieth century. The main purpose of the Percival mission to Mars is to collect and relay scientific data to Earth suitable for designing future manned and unmanned missions to Mars. The measurements and observations made by Percival will help future mission designers to choose among landing sites based on the feasibility and scientific interest of the sites. The primary measurements conducted by the Percival mission include gravity field determination, surface and atmospheric composition, sub-surface soil composition, sub-surface seismic activity, surface weather patterns, and surface imaging. These measurements will be taken from the orbiting Percival spacecraft and from surface penetrators deployed from Mars orbit. The design work for the Percival Mission to Mars was divided among four technical areas: Orbits and Propulsion System, Surface Penetrators, Gravity and Science Instruments, and Spacecraft Structure and Systems. The results for each of the technical areas is summarized and followed by a design cost analysis and recommendations for future analyses.

  7. Hematite on Mars!

    NASA Technical Reports Server (NTRS)

    2004-01-01

    This spectrum captured by the Mars Exploration Rover Opportunity's mini-thermal emission spectrometer shows the presence of grey hematite in the martian soil at Meridiani Planum, Mars. On Earth, hematite forms in the presence of water, at the bottom of lakes, springs and other bodies of standing water. But it can also arise without water in volcanic regions. Scientists hope to discover the origins of martian hematite with the help of Opportunity's robotic set of geological tools. The yellow line represents the spectrum, or light signature, of the martian soil, while the red line shows the spectrum of pure hematite.

  8. Terraforming earth and Mars

    NASA Technical Reports Server (NTRS)

    Levine, Joel S.

    1992-01-01

    The uncontrolled character of current earth environment changes ascribable to anthropogenic pollutants is presently contrasted with the prospects for a controlled, long-term program of 'terraforming' for Mars, whose culmination could be the introduction of organisms able to thrive in the new Martian environment in carefully designed ways. A detailed discussion is conducted concerning the chemical building-blocks available on Mars for this manner of 'environmental engineering', with frequent reference to comparable and contrasting features of the terrestrial surface, hydrosphere and atmosphere.

  9. Mars Obliquity Cycle Illustration

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The tilt of Mars' spin axis (obliquity) varies cyclically over hundreds of thousands of years, and affects the sunlight falling on the poles. Because the landing site of NASA's Phoenix Mars Lander is so near the north pole, higher sun and warmer temperatures during high obliquity lead to warmer, more humid surface environments, and perhaps thicker, more liquid-like films of water in soil.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  10. Mars Says 'hi'!

    NASA Technical Reports Server (NTRS)

    2004-01-01

    12 October 2004 Although one might argue that most of the 'i' is missing, and part of the 'h' has been eroded away, this Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows light-toned sedimentary rock outcrops in northern Sinus Meridiani that almost seem to spell out the word, 'hi'. This natural graffiti is all that remains of a suite of sedimentary rock that once covered the area shown here. The 400 meter scale bar is about 437 yards long. The features are located near 1.8oN, 357.2oW. Sunlight illuminates the scene from the upper left.

  11. Zapping Rocks on Mars

    ScienceCinema

    Wiens, Roger

    2016-07-12

    Better understanding Mars means better understanding its geology. That’s why, sitting atop NASA’s Curiosity rover, is ChemCam, an instrument built by Los Alamos National Laboratory that shoots lasers at Martian rocks and analyzes the data. After nearly 1,500 rock zaps, ChemCam has uncovered some surprising facts about the Red Planet, including the discovery of igneous rocks. Soon, a new Los Alamos-built instrument—the SuperCam—will ride aboard the Mars 2020 rover and bring with it enhanced capabilities to unlock new secrets about the planet.

  12. Zapping Rocks on Mars

    SciTech Connect

    Wiens, Roger

    2016-05-16

    Better understanding Mars means better understanding its geology. That’s why, sitting atop NASA’s Curiosity rover, is ChemCam, an instrument built by Los Alamos National Laboratory that shoots lasers at Martian rocks and analyzes the data. After nearly 1,500 rock zaps, ChemCam has uncovered some surprising facts about the Red Planet, including the discovery of igneous rocks. Soon, a new Los Alamos-built instrument—the SuperCam—will ride aboard the Mars 2020 rover and bring with it enhanced capabilities to unlock new secrets about the planet.

  13. Mars mission research center

    NASA Technical Reports Server (NTRS)

    1988-01-01

    The Mars Mission Research Center is one of nine University Space Engineering Research Centers established by NASA to broaden the nation's engineering capability to meet the critical needs of the civilian space program. It has the goal of focusing on research and training technologies for planetary exploration with particular emphasis on Mars. The research combines: (1) composite materials and fabrication, (2) light weight structures and controls, and (3) hypersonic aerodynamics and propulsion in a cross disciplined program directed towards the development of the space transportation system for planetary travel.

  14. Human exploration of Mars.

    PubMed

    Gwynne, O; McKay, C; Zubrin, R

    1991-06-01

    The human exploration of Mars has the potential to return a rich harvest of scientific information about that planet, its possible past biological history and the prospects for future habitation by Earthly life. The realization of that potential will require new approaches and new technologies--a whole new paradigm in space exploration. Picture yourself exploring the surface of Mars, where your task involves conducting a detailed investigation of features larger than the United States in order to uncover a record of planetary history spanning over four billion years.

  15. Frost on Mars

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image shows bluish-white frost seen on the Martian surface near NASA's Phoenix Mars Lander. The image was taken by the lander's Surface Stereo Imager on the 131st Martian day, or sol, of the mission (Oct. 7, 2008). Frost is expected to continue to appear in images as fall, then winter approach Mars' northern plains.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  16. Ferric sulfates on Mars

    NASA Technical Reports Server (NTRS)

    Burns, Roger G.

    1987-01-01

    Evidence is presented for the possible existence of ferric sulfato complexes and hydroxo ferric sulfate minerals in the permafrost of Mars. A sequential combination of ten unique conditions during the cooling history of Mars is suggested which is believed to have generated an environment within Martian permafrost that has stabilized Fe(3+)-SO4(2-)-bearing species. It is argued that minerals belonging to the jarosite and copiapite groups could be present in Martian regolith analyzed in the Viking XRF measurements at Chryse and Utopia, and that maghemite suspected to be coating the Viking magnet arrays is a hydrolysate of dissolved ferric sulfato complexes from exposed Martian permafrost.

  17. Iron Meteorite on Mars

    NASA Technical Reports Server (NTRS)

    2005-01-01

    NASA's Mars Exploration Rover Opportunity has found an iron meteorite on Mars, the first meteorite of any type ever identified on another planet. The pitted, basketball-size object is mostly made of iron and nickel. Readings from spectrometers on the rover determined that composition. Opportunity used its panoramic camera to take the images used in this approximately true-color composite on the rover's 339th martian day, or sol (Jan. 6, 2005). This composite combines images taken through the panoramic camera's 600-nanometer (red), 530-nanometer (green), and 480-nanometer (blue) filters.

  18. Sand and Dust on Mars

    NASA Technical Reports Server (NTRS)

    Greeley, Ronald; Haberle, Robert M.

    1991-01-01

    Mars is a planet of high scientific interest. Various studies are currently being made that involve vehicles that have landed on Mars. Because Mars is known to experience frequent wind storms, mission planners and engineers require knowledge of the physical and chemical properties of Martian windblown sand and dust, and the processes involved in the origin and evolution of sand and dust storms.

  19. Mars exploration: follow the water

    NASA Technical Reports Server (NTRS)

    Park, Young Ho

    2004-01-01

    Over the centuries, the red planet Mars has been a subject of imagination as well as intense scientific interest. As the overwhelming success of two Mars Exploration Rovers unfolds before us, this article provides an overview of and rationale for NASA's Mars exploration program.

  20. Lippia alba essential oil promotes survival of silver catfish (Rhamdia quelen) infected with Aeromonas sp.

    PubMed

    Sutili, Fernando J; Cunha, Mauro A; Ziech, Rosangela E; Krewer, Carina C; Zeppenfeld, Carla C; Heldwein, Clarissa G; Gressler, Leticia T; Heinzmann, Berta M; Vargas, Agueda C; Baldisserotto, Bernardo

    2015-03-01

    In vitro and in vivo activity of the Lippia alba essential oil (EO) against Aeromonas sp. was evaluated. In the in vitro assay the minimum inhibitory concentration (MIC) and a minimum bactericidal concentration (MBC) of EO for Aeromonas cells were determined using the microdilution method. Twenty five strains of Aeromonas sp. isolated from infected fish obtained from local fish farms were used. MIC and MBC values were 2862 and 5998 µg mL-1 for L. alba EO and 0.5 and 1.2 µg mL-1 for gentamicin, respectively. In the in vivo assay silver catfish juveniles (Rhamdia quelen) (7.50 ± 1.85 g and 10.0 ± 1.0 cm) with typical injuries associated to Aeromonas infection were divided into four treatments (in triplicate n=10): untreated fish (negative control), 10 mg L-1 of gentamicin, and 20 or 50 µL L-1 of EO. Fish were maintained in aerated 20 L plastic boxes. After 10 days survival of silver catfish infected with Aermonas sp. and treated with essential oil (50 µL L-1) was greater than 90%.

  1. Isolation and expression analysis of low temperature-induced genes in white poplar (Populus alba).

    PubMed

    Maestrini, Pierluigi; Cavallini, Andrea; Rizzo, Milena; Giordani, Tommaso; Bernardi, Rodolfo; Durante, Mauro; Natali, Lucia

    2009-09-15

    Poplar is an important crop and a model system to understand molecular processes of growth, development and responses to environmental stimuli in trees. In this study, we analyzed gene expression in white poplar (Populus alba) plants subjected to chilling. Two forward suppression-subtractive-hybridization libraries were constructed from P. alba plants exposed to low non-freezing temperature for 6 or 48h. Hundred and sixty-two cDNAs, 54 from the 6-h library and 108 from the 48-h library, were obtained. Isolated genes belonged to six categories of genes, specifically those that: (i) encode stress and defense proteins; (ii) are involved in signal transduction; (iii) are related to regulation of gene expression; (iv) encode proteins involved in cell cycle and DNA processing; (v) encode proteins involved in metabolism and energetic processes; and (vi) are involved in protein fate. Different expression patterns at 3, 6, 12, 24, 48h at 4 degrees C and after a recovery of 24h at 20 degrees C were observed for isolated genes, as expected according to the class in which the gene putatively belongs. Forty-four of 162 genes contained DRE/LTRE cis-elements in the 5' proximal promoter of their orthologs in Populus trichocarpa, suggesting that they putatively belong to the CBF regulon. The results contribute new data to the list of possible candidate genes involved in cold response in poplar.

  2. Alba Field cased hole horizontal gravel pack -- A team approach to design

    SciTech Connect

    Alexander, K.; Winton, S.; Price-Smith, C.

    1995-12-31

    A 700 ft. cased hole horizontal well was gravel packed and completed in the Alba Field, Central North Sea. The completion incorporated a number of new technologies adopted for a horizontal cased hole completion including both equipment and fluids. The zone was completed in 2 stages using a horizontal stack pack approach. Perforation packing was optimized by performing a staged acid prepack with the guns in the hole utilizing a low density synthetic gravel substitute in a shear thinning carrier fluid. This was a world first achievement at a cased hole gravel pack using the stack pack approach in a horizontal well. A solids free fluid loss control material was evaluated and chosen for the high permeability Alba sands (3 Darcy). Extensive lab testing was performed to ensure minimal damage from various fluids. A 30 ft. physical model was used to optimize annular pack efficiency. A gravel placement computer simulation was used to design pump rate, sand concentration and gel loading in order to optimize annular and perforation pack efficiency.

  3. Alba Field cased-hole horizontal gravel pack: A team approach to design

    SciTech Connect

    Alexander, K.; Winton, S.; Price-Smith, C.

    1996-03-01

    A 700-ft cased-hole horizontal well was gravel packed and completed in the Alba Field, central North Sea. The completion incorporated a number of new technologies adopted for a horizontal cased-hole completion, including both equipment and fluids. The zone was completed in two stages using a horizontal stack-pack approach. Perforation packing was optimized by performing a staged acid prepack with the guns in the hole using a low-density synthetic gravel substitute in a shear thinning carrier fluid. This was a world-first achievement at a cased-hole gravel pack using the stack-pack approach in a horizontal well. A solids-free fluid-loss control material was evaluated and chosen for the high-permeability Alba sands (3 darcies). Extensive lab testing was performed to ensure minimal damage from various fluids. A 30-ft physical model was used to optimize annular pack efficiency. A gravel placement computer simulation was used to design pump rate, sand concentration, and gel loading to optimize annular and perforation-pack efficiency.

  4. Alba field cased hole horizontal gravel pack -- a team approach to design

    SciTech Connect

    Alexander, K.; Winton, S.; Price-Smith, C.

    1995-12-31

    A 700 ft cased hole horizontal well was gravel packed and completed in the Alba Field, Central North Sea. The completion incorporated a number of new technologies adopted for a horizontal cased hole completion including both equipment and fluids. The zone was completed in 2 stages using a horizontal stack pack approach. Perforation packing was optimized by performing a staged acid prepack with the guns in the hole utilizing a low density synthetic gravel substitute in a shear thinning carrier fluid. This was a world first achievement at a cased hole gravel pack using the stack pack approach in a horizontal well. A solids free fluid loss control material was evaluated and chosen for the high permeability Alba Sands (3 Darcy). Extensive lab testing was performed to ensure minimal damage from various fluids. A 30 ft physical model was used to optimize annular pack efficiency. A gravel placement computer simulation was used to design pump rate, sand concentration and gel loading in order to optimize annular and perforation pack efficiency.

  5. Searching for ``Home Plates'' Near Gusev Crater, Mars: Spirit's Regional Context in an Area of Explosive Volcanism

    NASA Astrophysics Data System (ADS)

    Rice, M. S.; Batista, A. E.; Bell, J. F.; Watters, W. A.

    2010-12-01

    The Mars Exploration Rover (MER) Spirit has spent the last 4.5 years of its mission exploring the vicinity of a feature called Home Plate in the Columbia Hills of Gusev Crater, Mars. Home Plate is an 80m-wide plateau of layered, light-toned rocks interpreted to be a pyroclastic deposit based on its composition of altered alakali basaltic clastics, its enrichment in volatiles, and the presence of a bomb-sag. Discoveries of sulfate- and silica-rich soils and outcrops near Home Plate, as well as a geochemical gradient across Home Plate, suggest that alteration by hydrothermal fluids occurred at this site. However, probable source vents have not been found along Spirit’s traverse, and the spatial and temporal extents of pyroclastic activity in Gusev Crater are currently unknown. In this work, we test the hypothesis that explosive volcanism was widespread in the Gusev Crater region. We have performed a comprehensive photomorphologic survey of a 300km square region that includes Gusev Crater and the southern flank of Apollinaris Patera. Using images from the High Resolution Imaging Science Experiment (HiRISE) and Context Camera (CTX) onboard Mars Reconnaissance Orbiter (MRO), and from the Mars Orbital Camera (MOC) onboard Mars Global Surveyor (MGS), we have searched for “Home Plates,” possible vents, and other morphologic indicators of hydrovolcanic activity. We have identified 80+ quasi-circular, light-toned, layered features similar to Home Plate in hill structures above the Gusev lava plains, in the hummocky terrain SE of Thira Crater, and NW of Gusev in Zephyria Mensae. In some locations, these “Home Plates” are paired with conical structures (similar to the “von Braun” or “Goddard” features in the Columbia Hills). We have also performed a visible to near-infrared hyperspectral survey of the same region using data from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument on MRO. Seven high-resolution (18 m/pix) CRISM

  6. Mars Pathfinder and Mars Global Surveyor Outreach Compilation

    NASA Technical Reports Server (NTRS)

    1999-01-01

    This videotape is a compilation of the best NASA JPL (Jet Propulsion Laboratory) videos of the Mars Pathfinder and Mars Global Surveyor missions. The mission is described using animation and narration as well as some actual footage of the entire sequence of mission events. Included within these animations are the spacecraft orbit insertion; descent to the Mars surface; deployment of the airbags and instruments; and exploration by Sojourner, the Mars rover. JPL activities at spacecraft control during significant mission events are also included at the end. The spacecraft cameras pan the surrounding Mars terrain and film Sojourner traversing the surface and inspecting rocks. A single, brief, processed image of the Cydonia region (Mars face) at an oblique angle from the Mars Global Surveyor is presented. A description of the Mars Pathfinder mission, instruments, landing and deployment process, Mars approach, spacecraft orbit insertion, rover operation are all described using computer animation. Actual color footage of Sojourner as well as a 360 deg pan of the Mars terrain surrounding the spacecraft is provided. Lower quality black and white photography depicting Sojourner traversing the Mars surface and inspecting Martian rocks also is included.

  7. Mars One; creating a human settlement on Mars

    NASA Astrophysics Data System (ADS)

    Wielders, A.; Lansdorp, B.; Flinkenflögel, S.; Versteeg, B.; Kraft, N.; Vaandrager, E.; Wagensveld, M.; Dogra, A.; Casagrande, B.; Aziz, N.

    2013-09-01

    Mars One will take humanity to Mars in 2023, to establish a permanent settlement from which human kind will prosper, learn, and grow. Before the first crew lands, Mars One will have established a habitable, sustainable outpost designed to receive new astronauts every two years. To accomplish this, Mars One has developed a precise, realistic plan based entirely upon proven technologies. It is both economically and logistically feasible, and already underway with the aggregation and appointment of hardware suppliers and experts in space exploration. In this paper Mars One discusses the benefits of the mission for planetary science in general and Mars studies in particular. Furthermore potential contributions from the planetary community to the Mars One project will be identified.

  8. Mars Observer Orbit Insertion Briefing

    NASA Technical Reports Server (NTRS)

    1993-01-01

    Steve Wall is the host of this video entitled, "Return to the Red Planet". Live animation of the Mars Observer orbiting Mars is presented. Steve Wall explains the spacecraft insertion maneuver and also explains the purpose for the Mars Observer launch. Live coverage of the Cape Canaveral launch of the Mars Observer is also presented. Suzanne Dodd, Chief of the Mission Planning team describes the burn start and how the spacecraft will be captured by Mars' gravity. Glenn Cunningham, Mars Observer Project Manager, gives background information on the Mars Observer and describes the organizations behind the Mars Observer Spacecraft, such as the Deep Space Network, the Mission Operation Support Office, Science Investigators, the Flight Engineering Office, Operations Office, and the Ground Data System Office. Dr. William Piotrowski, Acting Director, Solar System Exploration Division, NASA, talks about the purpose of the Mars Pathfinder which is to develop the technology and systems for landing small science packages on Mars. Mr. Roger Gibbs, Former Mars Observer Spacecraft Systems Engineer, tells us how the Mars Observer was built and describes the structural elements on the Mars Observer. The 11-month cruise period for the spacecraft is given by Joseph Beerer, Manager of the Engineering office. The thrust for the Mars Orbit Insertion is described by Ronald Klemetson, Technical Manager, Propulsion Subsystem Jet Propulsion Laboratory (JPL). George Chen, Lead Engineer Attitude and Articulation Subsystem Spacecraft Team, explains the importance of the attitude control engines on the Spacecraft. Marvin Traxler, Manager of Tracking and Data Acquisition, describes how searching for a signal from the Mars Observer works. See NONP-NASA-VT-2000081555 for a continuation of this discussion with Marvin Traxler.

  9. Identifying rates of meadowfoam (Limnanthes alba) seed meal needed for suppression of Meloidogyne hapla and Pythium irregulare in soil

    Technology Transfer Automated Retrieval System (TEKTRAN)

    Meadowfoam (Limnanthes alba) is a commercial oilseed crop grown in Oregon. After extracting oil from seed, the remaining seed meal is rich in the secondary plant metabolite glucolimnanthin, which can be converted into pesticidal compounds such as 3-methoxybenzyl isothiocyanate (ITC) and 3-methoxyphe...

  10. Detoxification of semisolid olive-mill wastes and pine-chip mixtures using Phanerochaete flavido-alba.

    PubMed

    Linares, Araceli; Manuel Caba, Juan; Ligero, Francisco; de la Rubia, Teresa; Martínez, José

    2003-06-01

    Semisolid olive-mill residues, pine chips, and mixtures of both residues contain phytotoxic components capable of inhibiting germination and vegetative growth in plants. Solid-state cultures of Phanerochate flavido-alba on pine chips or mixtures of both residues reduce these phytotoxic effects in fermented substrates. The phenol and lipid contents in cultures detoxified by this fungus also decreases.

  11. Gas chromatograph analysis on closed air and nitrogen oxide storage atmospheres of recalcitrant seeds of Quercus Alba

    Technology Transfer Automated Retrieval System (TEKTRAN)

    Storage of recalcitrant seeds remains an unsolved problem. This study investigated the quantitative gas analysis of nitrous oxide (N2O) and air atmospheres on the recalcitrant seeds of Quercus alba by using gas chromatograph. Ten seeds were placed in each sealed atmospheric system of air and 98/2% N...

  12. Mars manned transportation vehicle

    NASA Technical Reports Server (NTRS)

    Perez-Davis, Marla E.; Faymon, Karl A.

    1987-01-01

    A viable power system technology for a surface transportation vehicle to explore the planet Mars is presented. A number of power traction systems were investigated, and it was found that a regenerative hydrogen-oxygen fuel cell appears to be attractive for a manned Mars rover application. Mission requirements were obtained from the Manned Mars Mission Working Group. Power systems weights, power, and reactants requirements were determined as a function of vehicle weights for vehicles weighing from 6,000 to 16,000 lb (2,722 to 7,257 kg), (Earth weight). The vehicle performance requirements were: velocity, 10 km/hr; range, 100 km; slope climbing capability, 30 deg uphill for 50 km; mission duration, 5 days; and crew, 5. Power requirements for the operation of scientific equipment and support system capabilities were also specified and included in this study. The concept developed here would also be applicable to a Lunar based vehicle for Lunar exploration. The reduced gravity on the Lunar surface, (over that on the Martian surface), would result in an increased range or capability over that of the Mars vehicle since many of the power and energy requirements for the vehicle are gravity dependent.

  13. Making Mars habitable.

    PubMed

    McKay, C P; Toon, O B; Kasting, J F

    1991-08-08

    Mars is believed to be lifeless, but it may be possible to transform it into a planet suitable for habitation by plants, and conceivably humans. The success of such an enterprise would depend on the abundance, distribution and form of materials on the planet that could provide carbon dioxide, water and nitrogen.

  14. The Phoenix Mars Mission

    NASA Technical Reports Server (NTRS)

    Tamppari, Leslie K.; Smith, Peter H.

    2008-01-01

    This slide presentation details the Phoenix Mission which was designed to enhance our understanding of water and the potential for habitability on the north polar regions of Mars. The slides show the instruments and the robotics designed to scrape Martian surface material, and analyze it in hopes of identifying water in the form of ice, and other chemicals.

  15. Mars landing site catalog

    NASA Technical Reports Server (NTRS)

    Greeley, Ronald (Editor)

    1990-01-01

    The catalog was compiled from material provided by the planetary community for areas on Mars that are of potential interest for future exploration. The catalog has been edited for consistency insofar as practical; however, the proposed scientific objectives and characteristics have not been reviewed. This is a working catalog that is being revised, updated, and expanded continually.

  16. Giant saltation on Mars

    PubMed Central

    Almeida, Murilo P.; Parteli, Eric J. R.; Andrade, José S.; Herrmann, Hans J.

    2008-01-01

    Saltation, the motion of sand grains in a sequence of ballistic trajectories close to the ground, is a major factor for surface erosion, dune formation, and triggering of dust storms on Mars. Although this mode of sand transport has been matter of research for decades through both simulations and wind tunnel experiments under Earth and Mars conditions, it has not been possible to provide accurate measurements of particle trajectories in fully developed turbulent flow. Here we calculate the motion of saltating grains by directly solving the turbulent wind field and its interaction with the particles. Our calculations show that the minimal wind velocity required to sustain saltation on Mars may be surprisingly lower than the aerodynamic minimal threshold measurable in wind tunnels. Indeed, Mars grains saltate in 100 times higher and longer trajectories and reach 5-10 times higher velocities than Earth grains do. On the basis of our results, we arrive at general expressions that can be applied to calculate the length and height of saltation trajectories and the flux of grains in saltation under various physical conditions, when the wind velocity is close to the minimal threshold for saltation. PMID:18443302

  17. Mars manned transportation vehicle

    SciTech Connect

    Perez-Davis, M.E.; Faymon, K.A.

    1987-07-01

    A viable power system technology for a surface transportation vehicle to explore the planet Mars is presented. A number of power traction systems were investigated, and it was found that a regenerative hydrogen-oxygen fuel cell appears to be attractive for a manned Mars rover application. Mission requirements were obtained from the Manned Mars Mission Working Group. Power systems weights, power, and reactants requirements were determined as a function of vehicle weights for vehicles weighing from 6,000 to 16,000 lb (2,722 to 7,257 kg), (Earth weight). The vehicle performance requirements were: velocity, 10 km/hr; range, 100 km; slope climbing capability, 30 deg uphill for 50 km; mission duration, 5 days; and crew, 5. Power requirements for the operation of scientific equipment and support system capabilities were also specified and included in this study. The concept developed here would also be applicable to a Lunar based vehicle for Lunar exploration. The reduced gravity on the Lunar surface, (over that on the Martian surface), would result in an increased range or capability over that of the Mars vehicle since many of the power and energy requirements for the vehicle are gravity dependent.

  18. Near-Mars space

    SciTech Connect

    Luhmann, J.G.; Brace, L.H. Michigan, University, Ann Arbor )

    1991-05-01

    The prevalent attributes of near-Mars space are described: the ambient interplanetary environment, the ionosphere, the upper atmosphere, and more remote regions that are affected by the presence of Mars. The descriptions are based on existing Martian data and/or models constructed from measurements made near Venus. Specific attention is given to the features of solar wind interaction with magnetospheric and ionospheric obstacles. The high-altitude plasma and field environment, the energetic particle environment, the ionosphere environment, and the neutral upper atmosphere environment are described with extensive graphic information, based on existing measurements collected from nine Martian missions. The ionospheric obstacle is assumed to prevail as a mechanism for describing the scenario. Martian perturbation of solar wind is theorized to be of a relatively small order. A distinctive local energetic particle population of planetary origin is shown to result from the direct interaction of solar wind plasma. This phenomenon is considered evidence of the important scavenging of planetary elements from Mars. The absence of a planetary dipole field around Mars, like its low gravity and distance from the sun, is considered important in determining the environment of this earthlike laboratory. 87 refs.

  19. Mars brine formation experiment

    NASA Technical Reports Server (NTRS)

    Moore, Jeffrey M.; Bullock, Mark A.; Stoker, Carol R.

    1992-01-01

    Evaporites, particularly carbonates, nitrates, and sulfates, may be major sinks of volatiles scavenged from the martian atmosphere. Mars is thought to have once had a denser, warmer atmosphere that permitted the presence of liquid surface water. The conversion of atmospheric CO2 into carbonate is hypothesized to have degraded the martian climate to its present state of a generally subfreezing, desiccated desert. The rate for such a conversion under martian conditions is poorly known, so the time scale of climate degradation by this process cannot be easily evaluated. If some models are correct, carbonate formation may have been fast at geological time scales. The experiments of Booth and Kieffer also imply fast (10(exp 6) - 10(exp 7) yr) removal of the missing CO2 inventory, estimated to be 1 - 5 bar, by means of carbonate formation. The timing of formation of many of the fluvial features observed on Mars is, in large part, dependent on when and how fast the atmosphere changed. A knowledge of the rate at which carbonates and nitrates formed is also essential for assessing the probability that life, or its chemical precursors, could have developed on Mars. No previous experiments have quantitatively evaluated the rate of solution for a suite of mobile anions and cations from unaltered minerals and atmospheric gases into liquid water under Mars-like conditions. Such experiments are the focus of this task.

  20. Mars: Cold and Wet

    NASA Astrophysics Data System (ADS)

    Fairén, A. G.; Davila, A. F.; Duport, L. G.; Amils, R.; McKay, C. P.

    2009-03-01

    The role of solutes depressing the melting point of water in a frozen martian environment supports the idea that the majority of the water on Mars was forming super-cooled liquid solutions with large masses of ice covering parts of them.

  1. Footprints on Mars

    NASA Technical Reports Server (NTRS)

    Drake, Bret G.

    2013-01-01

    The first three human missions to Mars should be to three different geographic sites. Maximize mobility to extend the reach of human exploration beyond the landing site. Maximize the amount of time that the astronauts spend exploring the planet. Provide subsurface access. Return a minimum of 250 kg of samples to Earth.

  2. Geologic Mapping of Mars

    NASA Astrophysics Data System (ADS)

    Price, Katherine H.

    1998-05-01

    Planetary geologic mapping involves integrating a terrestrial-based understanding of surface and subsurface processes and mapping principles to investigate scientific questions. Mars mappers must keep in mind that physical processes, such as wind and flowing water on Mars, are or were different from terrestrial processes because the planetary atmospheres have changed differently over time. Geologic mapping of Mars has traditionally been done by hand using overlays on photomosaics of Viking Orbiter and Mariner images. Photoclinometry and shadow measurements have been used to determine elevations, and the distribution and size of craters have been used to determine the relative ages of surfaces- more densely cratered surfaces are older. Some mappers are now using computer software (ranging from Photoshop to ArcInfo) to facilitate mapping, though their applications must be carefully executed so that registration of the images remains true. Images and some mapping results are now available on the internet, and new data from recent missions to Mars (Pathfinder and Surveyor) will offer clarifying information to mapping efforts. This paper consists chiefly of pictures and diagrams.

  3. Mars Express: exploration of Phobos

    NASA Technical Reports Server (NTRS)

    Duxbury, T. C.

    2001-01-01

    The ESA Mars Express Orbiter will be nearly polar and have an initial orbital period of 7.6 hours for the first 440 days and then will reduce its period to 6.7 hours. As periapsis of the elliptical orbit walks around Mars every 2 years, the ascending and descending nodes of the Mars Express orbit on the Mars equatorial plane will have the same radius as the orbit of Phobos and close encounters of Phobos will occur when Phobos is near the node as Mars Express passes.

  4. Recent Advances in Mars Tectonics

    NASA Technical Reports Server (NTRS)

    Golombek, M. P.; Banerdt, W. B.

    1999-01-01

    Since the publication of the "Stress and Tectonics on Mars" chapter in the Mars book (the last comprehensive summary of our knowledge on the topic) considerable advances have been made in certain areas of Martian tectonics and significant advances are expected with the return of Mars Global Surveyor data. This abstract will summarize the advances in our knowledge of tectonic features and processes on Mars since the Mars book and point towards new areas of research that can be expected from the Mars Global Surveyor data. Two out of three areas of study that were discussed as future directions of work in the Mars chapter have had significant work directed towards them. One area is the field of structural mapping and understanding the timing of tectonic activity on Mars in the framework of the global stratigraphy. Although the general development and relative timing of the development of the Tharsis province on Mars had been understood for some time, actual placement of mapped tectonic features in a global stratigraphic framework has only recently been completed. The second area of study mentioned in the Mars chapter was the impact of improved topography and gravity on modeling loads and deriving stresses in the Martian lithosphere. Mars Global Surveyor is on the brink of returning vastly improved topographic and gravity fields and these newer data sets can be used to better define the size and shape of Tharsis and to quantify loads and derived stresses in the Martian lithosphere. Additional information is contained in the original extended abstract.

  5. A calendar for Mars

    NASA Astrophysics Data System (ADS)

    Šuráň, Josef

    1997-06-01

    In a generalized approach to calendar construction for Earth, two types of perpetual calendars (with dates fixed to the days of a week) were studied for Mars: with leap and skip days; and with leap and skip weeks. Calendars with skip days or weeks (omitted days or weeks) are preferable, because the frequency of skip years is appreciably lower than that of leap years. Unlike our terrestrial (Gregorian) calendar with a 2-parametric leap rule (periods of 4 and 400 years), a Mars calendar of comparable accuracy requires a 3-parametric rule with three periods. The rules derived possess this accuracy and represent an optimum solution. With the skip week calendar, which appears to be the best compromise for a calendar for Mars, an error of 1 day would occur (theoretically) in an interval >100,000 Martian years. (However, unknown secular changes in the length of the Martian year, an inaccuracy in the adopted value of its length, and possible non-uniform rotation of Mars, may affect the calendar accuracy over such long intervals of time.) A common year would have 672 Martian days distributed into 24 months of 28 days (of 4 weeks of 7 days each). In skip years a week at the end of the twelfth month would be omitted. The above most regular arrangement of months (corresponding to 12 bi-months) and a 7 day Martian week, also offer the possibility of conveniently adapting terrestrial month and day names to the calendar of Mars. The month names could be, e.g. Januarione, Januaryide; Februarione, Februaryide, etc., and those for days, e.g. Mondim, Tuesdim, etc.

  6. Phoenix Lander on Mars

    NASA Technical Reports Server (NTRS)

    2007-01-01

    NASA's Phoenix Mars Lander monitors the atmosphere overhead and reaches out to the soil below in this artist's depiction of the spacecraft fully deployed on the surface of Mars.

    Phoenix has been assembled and tested for launch in August 2007 from Cape Canaveral Air Force Station, Fla., and for landing in May or June 2008 on an arctic plain of far-northern Mars. The mission responds to evidence returned from NASA's Mars Odyssey orbiter in 2002 indicating that most high-latitude areas on Mars have frozen water mixed with soil within arm's reach of the surface.

    Phoenix will use a robotic arm to dig down to the expected icy layer. It will analyze scooped-up samples of the soil and ice for factors that will help scientists evaluate whether the subsurface environment at the site ever was, or may still be, a favorable habitat for microbial life. The instruments on Phoenix will also gather information to advance understanding about the history of the water in the icy layer. A weather station on the lander will conduct the first study Martian arctic weather from ground level.

    The vertical green line in this illustration shows how the weather station on Phoenix will use a laser beam from a lidar instrument to monitor dust and clouds in the atmosphere. The dark 'wings' to either side of the lander's main body are solar panels for providing electric power.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems, Denver. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen (Denmark), the Max Planck Institute (Germany) and the Finnish Meteorological institute. JPL is a division of the California Institute of Technology in Pasadena.

  7. [MaRS Project

    NASA Technical Reports Server (NTRS)

    Aruljothi, Arunvenkatesh

    2016-01-01

    The Space Exploration Division of the Safety and Mission Assurances Directorate is responsible for reducing the risk to Human Space Flight Programs by providing system safety, reliability, and risk analysis. The Risk & Reliability Analysis branch plays a part in this by utilizing Probabilistic Risk Assessment (PRA) and Reliability and Maintainability (R&M) tools to identify possible types of failure and effective solutions. A continuous effort of this branch is MaRS, or Mass and Reliability System, a tool that was the focus of this internship. Future long duration space missions will have to find a balance between the mass and reliability of their spare parts. They will be unable take spares of everything and will have to determine what is most likely to require maintenance and spares. Currently there is no database that combines mass and reliability data of low level space-grade components. MaRS aims to be the first database to do this. The data in MaRS will be based on the hardware flown on the International Space Stations (ISS). The components on the ISS have a long history and are well documented, making them the perfect source. Currently, MaRS is a functioning excel workbook database; the backend is complete and only requires optimization. MaRS has been populated with all the assemblies and their components that are used on the ISS; the failures of these components are updated regularly. This project was a continuation on the efforts of previous intern groups. Once complete, R&M engineers working on future space flight missions will be able to quickly access failure and mass data on assemblies and components, allowing them to make important decisions and tradeoffs.

  8. Mars Surface Environmental Issues

    NASA Technical Reports Server (NTRS)

    Charles, John

    2002-01-01

    Planetary exploration by astronauts will require extended periods of habitation on a planet's surface, under the influence of environmental factors that are different from those of Earth and the spacecraft that delivered the crew to the planet. Human exploration of Mars, a possible near-term planetary objective, can be considered a challenging scenario. Mission scenarios currently under consideration call for surface habitation periods of from 1 to 18 months on even the earliest expeditions. Methods: Environmental issues associated with Mars exploration have been investigated by NASA and the National Space Biomedical Research Institute (NSBRI) as part of the Bioastronautics Critical Path Roadmap Project (see http ://criticalpath.jsc.nasa.gov). Results: Arrival on Mars will immediately expose the crew to gravity only 38% of that at Earth's surface in possibly the first prolonged exposure to gravity other than the 1G of Earth's surface and the zero G of weightless space flight, with yet unknown effects on crew physiology. The radiation at Mars' surface is not well documented, although the planet's bulk and even its thin atmosphere may moderate the influx of galactic cosmic radiation and energetic protons from solar flares. Secondary radiation from activated components of the soil must also be considered. Ultrafine and larger respirable and nonrespirable particles in Martian dust introduced into the habitat after surface excursions may induce pulmonary inflammation exacerbated by the additive reactive and oxidizing nature of the dust. Stringent decontamination cannot eliminate mechanical and corrosive effects of the dust on pressure suits and exposed machinery. The biohazard potential of putative indigenous Martian microorganisms may be assessed by comparison with analog environments on Earth. Even in their absence, human microorganisms, if not properly controlled, can be a threat to the crew's health. Conclusions: Mars' surface offers a substantial challenge to the

  9. Mars Science Laboratory at Canyon

    NASA Technical Reports Server (NTRS)

    2003-01-01

    December 2, 2003

    NASA's Mars Science Laboratory travels near a canyon on Mars in this artist's concept. The mission is under development for launch in 2009 and a precision landing on Mars in 2010.

    Once on the ground, the Mars Science Laboratory would analyze dozens of samples scooped up from the soil and cored from rocks as it explores with greater range than any previous Mars rover. It would investigate the past or present ability of Mars to support life. NASA is considering nuclear energy for powering the rover to give it a long operating lifespan.

    NASA's Jet Propulsion Laboratory, Pasadena, Calif., is managing development of the Mars Smart Laboratory for the NASA Office of Space Science, Washington, D.C.

  10. Exogenous stimulation with Eclipta alba promotes hair matrix keratinocyte proliferation and downregulates TGF-β1 expression in nude mice.

    PubMed

    Begum, Shahnaz; Lee, Mi Ra; Gu, Li Juan; Hossain, Jamil; Sung, Chang Keun

    2015-02-01

    Eclipta alba (L.) Hassk (E. alba) is a traditionally acclaimed medicinal herb used for the promotion of hair growth. However, to the best of our knowledge, no report has been issued to date on its effects on genetically distorted hair follicles (HFs). In this study, we aimed to identify an agent (stimuli) that may be beneficial for the restoration of human hair loss and which may be used as an alternative to synthetic drugs. We investigated the effects of petroleum ether extract (PEE) and different solvent fractions of E. alba on HFs of nude mice. Treatment was performed by topical application on the backs of nude mice and the changes in hair growth patterns were evaluated. Histological analysis was carried out to evaluate the HF morphology and the structural differences. Immunohistochemical (IHC) staining was performed to visualize follicular keratinocyte proliferation. The histological assessments revealed that the PEE-treated skin specimens exhibited prominent follicular hypertrophy. Subsequently, IHC staining revealed a significant increase (p<0.001) in the number of follicular keratinocytes in basal epidermal and matrix cells. Our results also demonstrated that PEE significantly (p<0.001) reduced the levels of transforming growth factor-β1 (TGF-β1) expression during early anagen and anagen-catagen transition. Our results suggest that PEE of E. alba acts as an important exogenous mediator that stimulates follicular keratinocyte proliferation and delays terminal differentiation by downregulating TGF-β1 expression. Thus, this study highlights the potential use of PEE of E. alba in the treatment of certain types of alopecia.

  11. Antidiabetic Effects of Aqueous Infusions of Artemisia herba-alba and Ajuga iva in Alloxan-Induced Diabetic Rats.

    PubMed

    Boudjelal, Amel; Siracusa, Laura; Henchiri, Cherifa; Sarri, Madani; Abderrahim, Benkhaled; Baali, Faiza; Ruberto, Giuseppe

    2015-06-01

    The aqueous infusions of the aerial parts of Artemisia herba-alba Asso and Ajuga iva Schreber, prepared in accordance with the traditional procedure used in the local folk medicine, have been analysed for their composition and content of phytochemical constituents and examined for their antidiabetic effectiveness in alloxan-induced diabetic rats. Oral administration of A. herba-alba and A. iva infusions was studied in normal and alloxan-induced diabetic rats, which were randomly divided into nine groups, each group consisting of six animals. The drug preparations (100, 200, and 300 mg/kg b. w.) of each plant were given orally to the rats of each group twice daily for 15 days. Compositional analysis of the aqueous infusions revealed the presence of several polyphenols as main components. A. herba-alba infusion was characterised by mono- and di-cinnamoylquinic acids, with 5-caffeoylquinic (chlorogenic) acid being the main compound, followed by 3,5-dicaffeoylquinic acid. Vicenin-2 (apigenin 6,8-di-C-glucoside) appeared to be the most abundant among flavonoids. On the other hand, A. iva showed the exclusive presence of flavonoids, with the flavanone naringin present in relatively high levels together with several apigenin (flavone) derivatives. Oral administration of 300 mg/kg b. w. of the aqueous infusions of A. herba-alba and A. iva exhibited a significant reduction in blood glucose content, showing a much more efficient antidiabetic activity compared to glibenclamide, the oral hypoglycaemic agent used as a positive control in this study. These results suggest that A. herba-alba and A. iva possess significant antidiabetic activity, as they were able to improve the biochemical damage in alloxan-induced diabetes in rats.

  12. Pre-sedation and transport of Rhamdia quelen in water containing essential oil of Lippia alba: metabolic and physiological responses.

    PubMed

    Becker, Alexssandro G; Parodi, Thaylise V; Zeppenfeld, Carla C; Salbego, Joseânia; Cunha, Mauro A; Heldwein, Clarissa G; Loro, Vania L; Heinzmann, Berta M; Baldisserotto, Bernardo

    2016-02-01

    The effects of transporting silver catfish (Rhamdia quelen) for 6 h in plastic bags containing 0 (control), 30 or 40 µL/L of essential oil (EO) from Lippia alba leaves were investigated. Prior to transport, the fish in the two experimental groups were sedated with 200 µL/L of EO for 3 min. After transport, dissolved oxygen, carbon dioxide, alkalinity, water hardness, pH, temperature and un-ionized ammonia levels in the transport water did not differ significantly among the groups. However, total ammonia nitrogen levels and net Na(+), Cl(-) and K(+) effluxes were significantly lower in the groups transported with EO of L. alba than those in the control group. PvO2, PvCO2 and HCO3(-) were higher after transporting fish in 40 µL/L of EO of L. alba, but there were no significant differences between groups regarding blood pH or hematocrit. Cortisol levels were significantly higher in fish transported in 30 µL/L of EO of L. alba compared to those of the control group. The metabolic parameters (glycogen, lactate, total amino acid, total ammonia and total protein) showed different responses after adding EO to the transport water. In conclusion, while the EO of L. alba is recommended for fish transport in the conditions tested in the present study because it was effective in reducing waterborne total ammonia levels and net ion loss, the higher hepatic oxidative stress in this species with the same EO concentrations reported by a previous study led us to conclude that the 10-20 µL/L concentration range of EO and lack of pre-sedation before transport are more effective.

  13. Life on Mars: Past, Present, and Future

    NASA Technical Reports Server (NTRS)

    McKay, Chris

    2006-01-01

    Mars has evidence for past liquid water, presence of an atmosphere with CO2 and N2, and potential for preservation of evidence of life. Composition of the Martian atmosphere is 95.3% Carbon dioxide, 2.7% Nitrogen, 1.6% Argon, 0.3-0.1% Water Vapor, 0.13% Oxygen, and 0.07% Carbon Monoxide. Current Mars missions include: Mars Global Surveyor, Mars Odyssey, Mars Exploration Rovers, Mars Express, and Mars Reconnaissance Orbiter,

  14. Developing an Updated, Integrated Understanding of Mars

    NASA Astrophysics Data System (ADS)

    Ehlmann, Bethany; Beaty, David; Meyer, Michael

    2014-09-01

    More than 650 scientists from 21 countries gathered in mid-July at the California Institute of Technology (Caltech) to debate and examine the status of our exploration of the Red Planet. Since the Seventh International Conference on Mars in 2007, seven Mars missions—Mars Odyssey, Mars Exploration Rovers (Spirit/Opportunity), Mars Express, Mars Reconnaissance Orbiter, Phoenix, and Mars Science Laboratory (Curiosity)—have been returning data, augmented by telescopic observations, studies of Martian meteorites, laboratory work, and modeling studies.

  15. Select problems in planetary structural geology: Global-scale tectonics on Io, regional-scale kinematics on Venus, and local-scale field analyses on Earth with application to Mars

    NASA Astrophysics Data System (ADS)

    Jaeger, Windy L.

    2005-11-01

    Io's mountains are cataloged in order to investigate their formation. Of the 101 mountains imaged with sufficient coverage and resolution for further analysis, 4 are volcanoes, and 97 are tectonic massifs. Of the 97 tectonic mountains, >=40 abut paterae (volcanic or volcano-tectonic depressions). This juxtaposition is unlikely to be coincidental as the probability of it occurring by chance is ~1.08%. The observed mountain-patera association may be due to orogenic faults acting as conduits for magma ascent, thus fueling patera formation near mountains. As resurfacing buries a shell of material from Io's surface to the base of the lithosphere, its effective radius is reduced and it heats up. The volume change due to subsidence and thermal expansion is calculated as a function of lithospheric thickness. Conservation of volume dictates that this material is uplifted at Io's surface. By estimating the total volume of mountains, Io's average lithospheric thickness is constrained to >=12 km. A kinematic analysis of Nefertiti Corona, Venus, reveals that the corona's interior moved east as a relatively coherent thrust sheet with most deformation occurring on the distal margin. Additionally, an en-echelon array indicates a history of semi-brittle deformation on the northern side of Nefertiti's tectonic annulus. Regional heating from the thermal diapir that formed Nefertiti probably reduced the crustal viscosity and enabled the semi-brittle deformation. The "Odessa Craters" in the Channeled Scabland of eastern Washington State are basaltic ring structures (BRSs) 50-500 m in diameter that are comprised of discontinuous, concentric outcrops of subvertically-jointed basalt and autointrusive basaltic dikes. It is postulated that they formed as follows: phreatovolcanic activity disrupted a relatively thin, active lava flow forming rootless cones; the lava flow inflated around the cones; tensile stresses caused concentric fracturing; dikes exploited the fractures and fed lava to

  16. Icebergs on early Mars

    NASA Astrophysics Data System (ADS)

    Uceda, E.; Fairen, A.; Woodworth-Lynas, C.; Palmero Rodriguez, A.

    2015-12-01

    The smooth topography of the Martian northern lowlands has been classically equated to an ancient ocean basin. The High-Resolution Imaging Science Experiment (HiRISE) onboard the Mars Reconnaissance Orbiter (MRO) is providing unprecedented images of the Martian surface at scales of 25 to 32 cm per pixel. The analysis of this high-resolution imaging reveals the presence of three differentiated geomorphologies throughout the northern lowlands of Mars and the Hellas basin, which are informative of the presence of icebergs floating in ancient oceans and/or seas. These morphologies are: (i) scattered scour marks, including curvilinear furrows several km long and some meters deep; (ii) boulders ranging in size from 0.5 m to ~2 m in diameter, distributed forming clusters with sizes from several hundred meters to 1-2 km; and (iii) flat-topped and conical circular fractured mounds. The association of plough marks, clusters of boulders and mounds on the northern plains of Mars can be related to the dual processes of ice keel scouring and ice rafting of both glacial and non-glacial detritus by a floating ice canopy and icebergs. These processes are well documented on Earth and result in distinct morphologies on the ocean floor, which are analogous to features observed in the Martian basins. Importantly, the features are located in elevated areas of the northern plains and Hellas, near the dichotomy boundary and on local topographic highs. Such distribution is expected, as these relatively shoal areas are where the iceberg-related features should occur on Mars: these areas had shallow water depths, less than the iceberg's keel depth, and therefore keels reached through the full depth of the water column to impinge on the sediments below. The presence of icebergs floating in cold oceans early in Mars' history imply the occurrence of continental glaciers forming in the highlands and streaming northward towards the lowlands, and towards the Hellas and Argyre Basins. Glacier

  17. Life sciences and space research XXIII(2): Planetary biology and origins of life; Proceedings of the Topical Meeting and Workshops XX, XXI and XXIII of the 27th COSPAR Plenary Meeting, Espoo, Finland, July 18-29, 1988

    NASA Technical Reports Server (NTRS)

    Schwartz, A. W. (Editor); Dose, K. (Editor); Raup, D. M. (Editor); Klein, H. P. (Editor); Devincenzi, D. L. (Editor)

    1989-01-01

    This volume includes chapters on exobiology in space, chemical and early biochemical evolution, life without oxygen, potential for chemical evolution in the early environment of Mars, planetary protection issues and sample return missions, and the modulation of biological evolution by astrophysical phenomena. Papers are presented on the results of spaceflight missions, the action of some factors of space medium on the abiogenic synthesis of nucleotides, early peptidic enzymes, microbiology and biochemistry of the methanogenic archaeobacteria, and present-day biogeochemical activities of anaerobic bacteria and their relevance to future exobiological investigations. Consideration is also given to the development of the Alba Patera volcano on Mars, biological nitrogen fixation under primordial Martian partial pressures of dinitrogen, the planetary protection issues in advance of human exploration of Mars, and the difficulty with astronomical explanations of periodic mass extinctions.

  18. Mars Science Laboratory (MSL) : the US 2009 Mars rover mission

    NASA Technical Reports Server (NTRS)

    Palluconi, Frank; Tampari, Leslie; Steltzner, Adam; Umland, Jeff

    2003-01-01

    The Mars Science Laboratory mission is the 2009 United States Mars Exploration Program rover mission. The MSL Project expects to complete its pre-Phase A definition activity this fiscal year (FY2003), investigations in mid-March 2004, launch in 2009, arrive at Mars in 2010 during Northern hemisphere summer and then complete a full 687 day Mars year of surface exploration. MSL will assess the potential for habitability (past and present) of a carefully selected landing region on Mars by exploring for the chemical building blocks of life, and seeking to understand quantitatively the chemical and physical environment with which these components have interacted over the geologic history of the planet. Thus, MSL will advance substantially our understanding of the history of Mars and potentially, its capacity to sustain life.

  19. Pityriasis alba

    MedlinePlus

    ... teens. It is more noticeable in children with dark skin. Symptoms The problem areas on the skin ( ... to the principles of the Health on the Net Foundation (www.hon.ch). The information provided herein ...

  20. New potential phytotherapeutics obtained from white mulberry (Morus alba L.) leaves.

    PubMed

    Gryn-Rynko, Anna; Bazylak, Grzegorz; Olszewska-Slonina, Dorota

    2016-12-01

    The present work demonstrates the profound and unique phyto-pharmacological and nutritional profile of white mulberry (Morus alba L.) leaves which containing considerable amounts of easy digestive proteins, carbohydrates, micro- and macronutrients, polyphenols, free amino acids, organic acids. The wide range of significant biopharmaceutical activities of the aqueous and polar organic solvents extracts from mulberry leaves - including antidiabetic, antibacterial, anticancer, cardiovascular, hypolipidemic, antioxidant, antiatherogenic, and anti-inflammatory - have been critically discussed. The main objective was to demonstrate the results of recently published study on the components of white mulberry leaves exhibiting their biological activity in the various pathological and health human ailments. In addition, we intend to drawn the attention of researchers and public health workers for the extended exploration of this deciduous plant leaves as the source of potential indigenous nutraceuticals and functional food products to enable development of alternative prevention and treatment protocols offered in therapy of the common non-communicable diseases and malignances.

  1. UV-B induced changes in the secondary metabolites of Morus alba L. leaves.

    PubMed

    Gu, Xi-Da; Sun, Ming-Yao; Zhang, Lin; Fu, Hong-Wei; Cui, Lei; Chen, Run-Ze; Zhang, Da-Wei; Tian, Jing-Kui

    2010-04-27

    Ultraviolet-B (UV-B) radiation is harmful to plants and human beings. Many secondary metabolites, like flavonoids, alkaloids, and lignin, are UV-B absorbing compounds, which can protect the genetic material of plants. Furthermore, they are active components of herbal drugs. UV-B radiation can activate the self-protective secondary metabolism system. The results of this paper provide a method to induce bioactive secondary metabolites from mulberry leaves (Morus alba L.) by UV-B irradiation in vitro. Five significantly different chromatographic peaks were found by HPLC fingerprint after induction, from which two active compounds were identified: One was chalcomoracin, a natural Diels-Alder type adduct with antibacterial activity; the other one was moracin N, which is a precursor of chalcomoracin. Their contents were 0.818 mg/g and 0.352 mg/g by dry weight, respectively.

  2. Fatty acids composition of Spanish black (Morus nigra L.) and white (Morus alba L.) mulberries.

    PubMed

    Sánchez-Salcedo, Eva M; Sendra, Esther; Carbonell-Barrachina, Ángel A; Martínez, Juan José; Hernández, Francisca

    2016-01-01

    This research has determined qualitatively and quantitatively the fatty acids composition of white (Morus alba) and black (Morus nigra) fruits grown in Spain, in 2013 and 2014. Four clones of each species were studied. Fourteen fatty acids were identified and quantified in mulberry fruits. The most abundant fatty acids were linoleic (C18:2), palmitic (C16:0), oleic (C18:1), and stearic (C18:0) acids in both species. The main fatty acid in all clones was linoleic (C18:2), that ranged from 69.66% (MN2) to 78.02% (MA1) of the total fatty acid content; consequently Spanish mulberry fruits were found to be rich in linoleic acid, which is an essential fatty acid. The fatty acid composition of mulberries highlights the nutritional and health benefits of their consumption.

  3. In vitro antimicrobial and cytotoxic activities of leaves and flowers extracts from Lippia alba.

    PubMed

    Ara, N; Nur, M H; Amran, M S; Wahid, M I I; Ahmed, M

    2009-01-01

    The research was conducted to investigate the in vitro antimicrobial and cytotoxic activities of leaves and flowers extract extracted from Lippia alba. Disc diffusion technique was used for in vitro antibacterial and antifungal screening. Zones of inhibition were observed in disc diffusion for antibacterial screening against 4 Gram-positive pathogenic and 6 Gram-negative pathogenic bacteria. Among crude extracts chloroform extract showed good activity against all test organisms. A Large zone of inhibition was observed (18 mm) against Vibrio parahaemolyticus. In antifungal screening, the compound showed mild to moderate zones of inhibition against four tested organisms. A Large zone of inhibition was observed against Aspergillus niger (13 mm). Cytotoxic activities of crude extracts were determined using Brine shrimp lethality Bioassay and LC50 values of standard Vincristin sulphate as positive control, n-hexane and crude ethanol extracts were found to be 5, 15 and 20 microg mL(-1), respectively.

  4. Effects of Applied Nitrogen Amounts on the Functional Components of Mulberry (Morus alba L.) Leaves.

    PubMed

    Sugiyama, Mari; Takahashi, Makoto; Katsube, Takuya; Koyama, Akio; Itamura, Hiroyuki

    2016-09-21

    This study investigated the effects of applied nitrogen amounts on specific functional components in mulberry (Morus alba L.) leaves. The relationships between mineral elements and the functional components in mulberry leaves were examined using mulberry trees cultivated in different soil conditions in four cultured fields. Then, the relationships between the nitrogen levels and the leaf functional components were studied by culturing mulberry in plastic pots and experimental fields. In the common cultured fields, total nitrogen was negatively correlated with the chlorogenic acid content (R(2) = -0.48) and positively correlated with the 1-deoxynojirimycin content (R(2) = 0.60). Additionally, differences in nitrogen fertilizer application levels affected each functional component in mulberry leaves. For instance, with increased nitrogen levels, the chlorogenic acid and flavonol contents significantly decreased, but the 1-deoxynojirimycin content significantly increased. Selection of the optimal nitrogen application level is necessary to obtain the desired functional components from mulberry leaves.

  5. Antidiabetic and antioxidant effects and phytochemicals of mulberry fruit (Morus alba L.) polyphenol enhanced extract.

    PubMed

    Wang, Yihai; Xiang, Limin; Wang, Chunhua; Tang, Chao; He, Xiangjiu

    2013-01-01

    The antidiabetic and antioxidant activities of the ethyl acetate-soluble extract (MFE) of mulberry fruit (Morus alba L.) were investigated. In vitro, MFE showed potent α-glucosidase inhibitory activity and radical-scavenging activities against DPPH and superoxide anion radicals. In vivo, MFE could significantly decrease fasting blood glucose (FBG) and glycosylated serum protein (GSP), and increase antioxidant enzymatic activities (SOD, CAT, GSH-Px) in streptozotocin (STZ)-induced diabetic mice. Bioactivity-guided fractionation of the MFE led to the isolation of 25 phenolic compounds, and their structures were identified on the basis of MS and NMR data. All the 25 compounds were isolated from mulberry fruit for the first time. Also, the α-glucosidase inhibitory activity and antioxidant activity of the phenolics were evaluated. Potent α-glucosidase inhibitory and radical-scavenging activities of these phenolics suggested that they may be partially responsible for the antidiabetic and antioxidant activities of mulberry fruit.

  6. Trends in North American small mammals found in common barn-owl (Tyto alba) dietary studies

    USGS Publications Warehouse

    Clark, D.R.; Bunck, C.M.

    1991-01-01

    Data on mammals were compiled from published studies of common barn-owl (Tyto alba) pellets. Mammalian composition of pellet samples was analyzed within geographic regions in regard to year, mean annual precipitation, latitude, and number of individual mammals in the sample. Percentages of individuals in pellets that were shrews increased whereas the percentages of rodents decreased with greater mean annual precipitation, especially in northern and western areas of North America. From the 1920s through 1980s, in northern and eastern areas the percentage of species that was shrews decreased, and in northern and central areas the percentage of individuals that was murid rats and mice increased. Human alterations of habitats during these seven decades are postulated to have caused changes in available small mammals, leading to changes in the barn-owl diet.

  7. New methodologies for the extraction and fractionation of bioactive carbohydrates from mulberry (Morus alba) leaves.

    PubMed

    Rodríguez-Sánchez, Sonia; Ruiz-Aceituno, Laura; Sanz, María L; Soria, Ana C

    2013-05-15

    Pressurized liquid extraction (PLE) was applied for the first time to extract bioactive low molecular weight carbohydrates (iminosugars and inositols) from mulberry ( Morus alba ) leaves. Under optimized conditions, PLE provided a similar yield to the conventional process used to extract these bioactives, but in less time (5 vs 90 min). To remove carbohydrates that interfere with the bioactivity of iminosugars from PLE extracts, two fractionation treatments were evaluated: yeast ( Saccharomyces cerevisiae ) incubation and cation-exchange chromatography (CEC). Both methods allowed complete removal of major soluble carbohydrates (fructose, glucose, galactose, and sucrose), without affecting the content of mulberry bioactives. As an advantage over CEC, the yeast treatment preserves bioactive inositols, and it is an affordable methodology that employs food grade solvents. This work found PLE followed by yeast treatment to be an easily scalable and automatable procedure that can be implemented in the food industry.

  8. Antidiabetic and Antioxidant Effects and Phytochemicals of Mulberry Fruit (Morus alba L.) Polyphenol Enhanced Extract

    PubMed Central

    Wang, Yihai; Xiang, Limin; Wang, Chunhua; Tang, Chao; He, Xiangjiu

    2013-01-01

    The antidiabetic and antioxidant activities of the ethyl acetate-soluble extract (MFE) of mulberry fruit (Morus alba L.) were investigated. In vitro, MFE showed potent α-glucosidase inhibitory activity and radical-scavenging activities against DPPH and superoxide anion radicals. In vivo, MFE could significantly decrease fasting blood glucose (FBG) and glycosylated serum protein (GSP), and increase antioxidant enzymatic activities (SOD, CAT, GSH-Px) in streptozotocin (STZ)-induced diabetic mice. Bioactivity-guided fractionation of the MFE led to the isolation of 25 phenolic compounds, and their structures were identified on the basis of MS and NMR data. All the 25 compounds were isolated from mulberry fruit for the first time. Also, the α-glucosidase inhibitory activity and antioxidant activity of the phenolics were evaluated. Potent α-glucosidase inhibitory and radical-scavenging activities of these phenolics suggested that they may be partially responsible for the antidiabetic and antioxidant activities of mulberry fruit. PMID:23936259

  9. The Exploration of Mars by Humans: Why Mars? Why Humans?

    NASA Technical Reports Server (NTRS)

    Levine, Joel S.

    2011-01-01

    As we commemorate the 50th anniversary of Yuri Gagarin's historic flight in 1961, the first flight of a human in space, plans are underway for another historic human mission. Plans are being developed for a human mission to Mars. Once we reach Mars, the human species will become the first two-planet species. Both the Bush Administration (in 2004) and the Obama Administration (in 2010) proposed a human mission to Mars as a national goal of the United States.

  10. Happy Mars Solstice!

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image was acquired by NASA's Phoenix Mars Lander's Surface Stereo Imager (SSI) in the late afternoon of the 30th Martian day of the mission, or Sol 30 (June 25, 2008). This is hours after the beginning of Martian northern summer. SSI used its natural-color filters, therefore the color is the color you would see on Mars. The image shows shadows from the SSI (left) and from the meteorological station mast (right) stretching toward the east as the sun dropped low in the west.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is led by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver

  11. Artificial structures on Mars

    NASA Astrophysics Data System (ADS)

    Van Flandern, T.

    2002-05-01

    Approximately 70,000 images of the surface of Mars at a resolution of up to 1.4 meters per pixel, taken by the Mars Global Surveyor spacecraft, are now in public archives. Approximately 1% of those images show features that can be broadly described as `special shapes', `tracks, trails, and possible vegetation', `spots, stripes, and tubes', `artistic imagery', and `patterns and symbols'. Rather than optical illusions and tricks of light and shadow, most of these have the character that, if photographed on Earth, no one would doubt that they were the products of large biology and intelligence. In a few cases, relationships, context, and fulfillment of a priori predictions provide objective evidence of artificiality that is exempt from the influence of experimenter biases. Only controlled test results can be trusted because biases are strong and operate both for and against artificiality.

  12. Mars Microprobe Entry Analysis

    NASA Technical Reports Server (NTRS)

    Braun, Robert D.; Mitcheltree, Robert A.; Cheatwood, F. McNeil

    1998-01-01

    The Mars Microprobe mission will provide the first opportunity for subsurface measurements, including water detection, near the south pole of Mars. In this paper, performance of the Microprobe aeroshell design is evaluated through development of a six-degree-of-freedom (6-DOF) aerodynamic database and flight dynamics simulation. Numerous mission uncertainties are quantified and a Monte-Carlo analysis is performed to statistically assess mission performance. Results from this 6-DOF Monte-Carlo simulation demonstrate that, in a majority of the cases (approximately 2-sigma), the penetrator impact conditions are within current design tolerances. Several trajectories are identified in which the current set of impact requirements are not satisfied. From these cases, critical design parameters are highlighted and additional system requirements are suggested. In particular, a relatively large angle-of-attack range near peak heating is identified.

  13. 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.

  14. Geophysics of Mars

    NASA Technical Reports Server (NTRS)

    Wells, R. A.

    1979-01-01

    A physical model of Mars is presented on the basis of light-scattering observations of the Martian atmosphere and surface and interior data obtained from observations of the geopotential field. A general description of the atmosphere is presented, with attention given to the circulation and the various cloud types, and data and questions on the blue haze-clearing effect and the seasonal darkening wave are summarized and the Mie scattering model developed to explain these observations is presented. The appearance of the planet from earth and spacecraft through Mariner 9 is considered, and attention is given to the preparation of topographical contour maps, the canal problem and large-scale lineaments observed from Mariner 9, the gravity field and shape of the planet and the application of Runcorn's geoid/convection theory to Mars. Finally, a summary of Viking results is presented and their application to the understanding of Martian geophysics is discussed.

  15. Mars - A contamination potential?

    NASA Technical Reports Server (NTRS)

    Huguenin, R. L.; Miller, K. J.; Leschine, S. B.

    1983-01-01

    Three regions on Mars, Solis Lacus, Noachis-Hellespontus, and the Syrtis Major border areas, would appear to have generally less hostile environments than at the Viking lander sites. Significant soil moisture may extend to within about 1 cm of the surface. Water vapor pressures within the pore spaces may be near saturation, and brines may be physically segregated from pockets of relatively pure H2O. Temperatures reach above 0 C during southern spring and summer, with peak temperatures reaching +22 C. These regions should contain fewer oxidants, and primary synthesis of organics may occur. The potential for contamination of these sites by microbes transported from existing spacecraft should be assessed. The adequacy of proposed new planetary protection procedures for possible future United States Mars Surface Sample Return missions should also be assessed in light of these findings.

  16. The soils of Mars

    NASA Technical Reports Server (NTRS)

    Banin, A.

    1988-01-01

    A mineralogical model for the Mars fine soil that includes as major components smectite clays absorbed and coated with amorphous iron oxyhydroxides and perhaps mixed with small amounts of better-crystalized iron oxides as separate phases is proposed. Also present as accessory minerals are sulfate minerals such as kieserite (MgSO4.H2O) and/or anhydrite (CaSO4), rutile (TiO2), and maghemite (Fe2O3) or magnetite (Fe3O4), the last two as magnetic components. Carbonates may be present at low concentrations only (less than 1 to 2 pct). However, a prime question to be addressed by a Mars Sample Return Mission shall be related to the mineralogical composition of the soil, and its spatial variability.

  17. Fossil life on Mars

    NASA Technical Reports Server (NTRS)

    Walter, M. R.

    1989-01-01

    Three major problems beset paleontologists searching for morphological evidence of life on early Earth: selecting a prospective site; finding biogenic structures; and distinguishing biogenic from abiogenic structures. The same problems arise on Mars. Terrestrial experience suggests that, with the techniques that can be employed remotely, ancient springs, including hot springs, are more prospective than lake deposits. If, on the other hand, the search is for chemical evidence, the strategy can be very different, and lake deposits are attractive targets. Lakes and springs frequenly occur in close proximity, and therefore a strategy that combines the two would seem to maximize the chance of success. The strategy for a search for stromatolite on Mars is discussed.

  18. The politics of Mars

    NASA Technical Reports Server (NTRS)

    Schmitt, Harrison H.

    1986-01-01

    A discussion is presented comparing past and present major accomplishments of the U.S. and the Soviet Union in space. It concludes that the Soviets are presently well ahead of the U.S. in several specific aspects of space accomplishment and speculates that the Soviet strategy is directed towards sending a man to the vicinity of Mars by the end of this century. A major successful multinational space endeavor, INTELSAT, is reviewed and it is suggested that the manned exploration of Mars offers a unique opportunity for another such major international cooperative effort. The current attitude of U.S. leadership and the general public is assessed as uniformed or ambivalent about the perceived threat of Soviet dominance in space.

  19. Mars Climate Orbiter

    NASA Technical Reports Server (NTRS)

    1998-01-01

    The purpose of this mission is to study the climate history and the water distribution of Mars. Beautiful panoramic views of the shuttle on the launch pad, engine ignition, Rocket launch, and the separation and burnout of the Solid Rocket Boosters are shown. The footage also includes an animation of the mission. Detailed views of the path that the Orbiter traversed were shown. Once the Orbiter lands on the surface of Mars, it will dig a six to eight inch hole and collect samples from the planets' surface. The animation also included the prospective return of the Orbiter to Earth over the desert of Utah. The remote sensor on the Orbiter helps in finding the exact location of the Orbiter so that scientists may collect the sample and analyze it.

  20. MARS Mission research center

    NASA Technical Reports Server (NTRS)

    1991-01-01

    The Mars Mission Research Center (M2RC) is one of nine University Space Engineering Research Centers established by NASA in June 1988. It is a cooperative effort between NCSU and A&T in Greensboro. The goal of the Center is to focus on research and educational technologies for planetary exploration with particular emphasis on Mars. The research combines Mission Analysis and Design, Hypersonic Aerodynamics and Propulsion, Structures and Controls, Composite Materials, and Fabrication Methods in a cross-disciplined program directed towards the development of space transportation systems for lunar and planetary travel. The activities of the students and faculty in the M2RC for the period 1 Jul. 1990 to 30 Jun. 1991 are described.

  1. Seismology on Mars

    NASA Technical Reports Server (NTRS)

    Anderson, D. L.; Miller, W. F.; Latham, G. V.; Nakamura, Y.; Toksoz, M. N.; Dainty, A. M.; Duennebier, F. K.; Lazarewicz, A. R.; Kovach, R. L.; Knight, T. C. D.

    1977-01-01

    High-quality data (uncontaminated by lander or wind noise) obtained with a three-axis short-period seismometer operating on Mars in the Utopia Planitia region are analyzed. No large events have been detected during the first five months of operation covered in the present paper. This indicates that Mars is less seismically active than the earth. Winds, and therefore a seismic background, began to intrude into the nighttime hours, starting with sol 119 (sol is a Martian day). The seismic background correlates well with wind velocity, and is proportional to the square of the wind velocity, as is appropriate for turbulent flow. A local seismic event of a magnitude of 3 and a distance of 110 km was detected on sol 80. It is interpreted as a natural seismic event.

  2. Mars Science Laboratory Drill

    NASA Technical Reports Server (NTRS)

    Okon, Avi B.

    2010-01-01

    The Drill for the Mars Science Laboratory mission is a rotary-percussive sample acquisition device with an emphasis on toughness and robustness to handle the harsh environment on Mars. The unique challenges associated with autonomous drilling from a mobile robot are addressed. A highly compressed development schedule dictated a modular design architecture that satisfies the functional and load requirements while allowing independent development and testing of the Drill subassemblies. The Drill consists of four actuated mechanisms: a spindle that rotates the bit, a chuck that releases and engages bits, a novel voice-coil-based percussion mechanism that hammers the bit, and a linear translation mechanism. The Drill has three passive mechanisms: a replaceable bit assembly that acquires and collects sample, a contact sensor / stabilizer mechanism, and, lastly a flex harness service loop. This paper describes the various mechanisms that makeup the Drill and discusses the solutions to their unique design and development challenges.

  3. MSATT Workshop on Chemical Weathering on Mars

    NASA Technical Reports Server (NTRS)

    Burns, Roger (Editor); Banin, Amos (Editor)

    1992-01-01

    The topics covered with respect to chemical weathering on Mars include the following: Mars soil, mineralogy, spectroscopic analysis, clays, silicates, oxidation, iron oxides, water, chemical reactions, geochemistry, minerals, Mars atmosphere, atmospheric chemistry, salts, planetary evolution, volcanology, Mars volcanoes, regolith, surface reactions, Mars soil analogs, carbonates, meteorites, and reactivity.

  4. MARS Flight Engineering Status

    SciTech Connect

    Fast, James E.; Dorow, Kevin E.; Morris, Scott J.; Thompson, Robert C.; Willett, Jesse A.

    2010-04-06

    The Multi-sensor Airborne Radiation Survey Flight Engineering project (MARS FE) has designed a high purity germanium (HPGe) crystal array for conducting a wide range of field measurements. In addition to the HPGe detector system, a platform-specific shock and vibration isolation system and environmental housing have been designed to support demonstration activities in a maritime environment on an Unmanned Surface Vehicle (USV). This report describes the status of the equipment as of the end of FY09.

  5. Powering Mars Rovers

    SciTech Connect

    Stewert, Robin

    2010-01-01

    INL scientists are doing their best to help solve our energy problems here on Earth. But did you know the lab is playing a key role in the exploration of other worlds, too? Meet INL Engineer Robin Stewart helps build and test generators that power NASA missions to Pluto and Mars. You can learn more about INL projects at http://www.facebook.com/idahonationallaboratory.

  6. Powering Mars Rovers

    ScienceCinema

    Stewert, Robin

    2016-07-12

    INL scientists are doing their best to help solve our energy problems here on Earth. But did you know the lab is playing a key role in the exploration of other worlds, too? Meet INL Engineer Robin Stewart helps build and test generators that power NASA missions to Pluto and Mars. You can learn more about INL projects at http://www.facebook.com/idahonationallaboratory.

  7. Organics on Mars?

    PubMed

    ten Kate, Inge L

    2010-01-01

    Organics are expected to exist on Mars based on meteorite infall, in situ production, and any possible biological sources. Yet they have not been detected on the martian surface; are they there, or are we not capable enough to detect them? The Viking gas chromatograph-mass spectrometer did not detect organics in the headspace of heated soil samples with a detection limit of parts per billion. This null result strongly influenced the interpretation of the reactivity seen in the Viking biology experiments and led to the conclusion that life was not present and, instead, that there was some chemical reactivity in the soil. The detection of perchlorates in the martian soil by instruments on the Phoenix lander and the reports of methane in the martian atmosphere suggest that it may be time to reconsider the question of organics. The high-temperature oxidizing properties of perchlorate will promote combustion of organics in pyrolytic experiments and may have affected the ability of both Phoenix's organic analysis experiment and the Viking mass spectrometer experiments to detect organics. So the question of organics on Mars remains open. A primary focus of the upcoming Mars Science Laboratory will be the detection and identification of organic molecules by means of thermal volatilization, followed by gas chromatography-mass spectrometry--as was done on Viking. However, to enhance organic detectability, some of the samples will be processed with liquid derivatization agents that will dissolve organics from the soil before pyrolysis, which may separate them from the soil perchlorates. Nonetheless, the problem of organics on Mars is not solved, and for future missions other organic detection techniques should therefore be considered as well.

  8. Mars Miniature Science Instruments

    NASA Technical Reports Server (NTRS)

    Kim, Soon Sam; Hayati, Samad; Lavery, David; McBrid, Karen

    2006-01-01

    For robotic Mars missions, all the science information is gathered through on-board miniature instruments that have been developed through many years of R&D. Compared to laboratory counterparts, the rover instruments require miniaturization, such as low mass (1-2 kg), low power (> 10 W) and compact (1-2 liter), yet with comparable sensitivity. Since early 1990's, NASA recognized the need for the miniature instruments and launched several instrument R&D programs, e.g., PIDDP (Planetary Instrument Definition and Development). However, until 1998, most of the instrument R&D programs supported only up to a breadboard level (TRL 3, 4) and there is a need to carry such instruments to flight qualifiable status (TU 5, 6) to respond to flight AOs (Announcement of Opportunity). Most of flight AOs have only limited time and financial resources, and can not afford such instrument development processes. To bridge the gap between instrument R&D programs and the flight instrument needs, NASA's Mars Technology Program (MTP) created advanced instrumentation program, Mars Instrument Development Project (MIDP). MIDP candidate instruments are selected through NASA Research Announcement (NRA) process [l]. For example, MIDP 161998-2000) selected and developed 10 instruments, MIDP II (2003-2005) 16 instruments, and MIDP III (2004-2006) II instruments.Working with PIs, JPL has been managing the MIDP tasks since September 1998. All the instruments being developed under MIDP have been selected through a highly competitive NRA process, and employ state-of-the-art technology. So far, four MIDP funded instruments have been selected by two Mars missions (these instruments have further been discussed in this paper).

  9. Cryptic Terrain on Mars

    NASA Technical Reports Server (NTRS)

    2007-01-01

    [figure removed for brevity, see original site] Figure 1

    There is an enigmatic region near the south pole of Mars known as the 'cryptic' terrain. It stays cold in the spring, even as its albedo darkens and the sun rises in the sky.

    This region is covered by a layer of translucent seasonal carbon dioxide ice that warms and evaporates from below. As carbon dioxide gas escapes from below the slab of seasonal ice it scours dust from the surface. The gas vents to the surface, where the dust is carried downwind by the prevailing wind.

    The channels carved by the escaping gas are often radially organized and are known informally as 'spiders' (figure 1).

    Observation Geometry Image PSP_003179_0945 was taken by the High Resolution Imaging Science Experiment (HiRISE) camera onboard the Mars Reconnaissance Orbiter spacecraft on 01-Apr-2007. The complete image is centered at -85.4 degrees latitude, 104.0 degrees East longitude. The range to the target site was 245.9 km (153.7 miles). At this distance the image scale is 49.2 cm/pixel (with 2 x 2 binning) so objects 148 cm across are resolved. The image shown here has been map-projected to 50 cm/pixel . The image was taken at a local Mars time of 06:19 PM and the scene is illuminated from the west with a solar incidence angle of 78 degrees, thus the sun was about 12 degrees above the horizon. At a solar longitude of 210.8 degrees, the season on Mars is Northern Autumn.

  10. Mars Rover RTG Study

    SciTech Connect

    Schock, Alfred

    1989-08-25

    This report summarizes the results of a Radioisotope Thermoelectric Generator (RTG) design study conducted by Fairchild Space Company at the direction of the U.S. Department of Energy's Office of SpecialApplications, in suppport of the Mars Rover and Sample Return mission under investigation at NASA's Jet Propulsion Laboratory. The report is a rearranged, updated, and significantly expanded amalgam of three interrelated papers presented at the 24th Intersocity Energy Conversion Engineering Conference (IECEC) at Arlington, Virginia, on August 10, 1989.

  11. Climate Change on Mars

    NASA Technical Reports Server (NTRS)

    Haberle, R. M.; Cuzzi, Jeffrey N. (Technical Monitor)

    1994-01-01

    Today, Mars is cold and dry. With a 7 mbar mean surface pressure, its thin predominantly CO2 atmosphere is not capable of raising global mean surface temperatures significantly above its 217K effective radiating temperature, and the amount of water vapor in the atmosphere is equivalent to a global ocean only 10 microns deep. Has Mars always been in such a deep freeze? There are several lines of evidence that suggest it has not. First, there are the valley networks which are found throughout the heavily cratered terrains. These features are old (3.8 Gyr) and appear to require liquid water to form. A warm climate early in Mars' history has often been invoked to explain them, but the precise conditions required to achieve this have yet to be determined. Second, some of the features seen in orbiter images of the surface have been interpreted in terms of glacial activity associated with an active hydrological cycle some several billion years ago. This interpretation is controversial as it requires the release of enormous quantities of ground water and enough greenhouse warming to raise temperatures to the melting point. Finally, there are the layered terrains that characterize both polar regions. These terrains are geologically young (10 Myr) and are believed to have formed by the slow and steady deposition of dust and water ice from the atmosphere. The individual layers result from the modulation of the deposition rate which is driven by changes in Mars' orbital parameters. The ongoing research into each of these areas of Martian climate change will be reviewed, and similarities to the Earth's climate system will be noted.

  12. Ice on Mars Again

    NASA Technical Reports Server (NTRS)

    1979-01-01

    This high resolution photo of the surface of Mars was taken by Viking Lander 2 at its Utopia Planitia landing site on May 18, 1979, and relayed to Earth by Orbiter 1 on June 7th. It shows a thin coating of water ice on the rocks and soil. The time of the frost appearance corresponds almost exactly with the build up of frost one Martian year (23 Earth Months) ago.

  13. Organics on Mars?

    NASA Astrophysics Data System (ADS)

    ten Kate, Inge L.

    2010-08-01

    Organics are expected to exist on Mars based on meteorite infall, in situ production, and any possible biological sources. Yet they have not been detected on the martian surface; are they there, or are we not capable enough to detect them? The Viking gas chromatograph-mass spectrometer did not detect organics in the headspace of heated soil samples with a detection limit of parts per billion. This null result strongly influenced the interpretation of the reactivity seen in the Viking biology experiments and led to the conclusion that life was not present and, instead, that there was some chemical reactivity in the soil. The detection of perchlorates in the martian soil by instruments on the Phoenix lander and the reports of methane in the martian atmosphere suggest that it may be time to reconsider the question of organics. The high-temperature oxidizing properties of perchlorate will promote combustion of organics in pyrolytic experiments and may have affected the ability of both Phoenix's organic analysis experiment and the Viking mass spectrometer experiments to detect organics. So the question of organics on Mars remains open. A primary focus of the upcoming Mars Science Laboratory will be the detection and identification of organic molecules by means of thermal volatilization, followed by gas chromatography - mass spectrometry - as was done on Viking. However, to enhance organic detectability, some of the samples will be processed with liquid derivatization agents that will dissolve organics from the soil before pyrolysis, which may separate them from the soil perchlorates. Nonetheless, the problem of organics on Mars is not solved, and for future missions other organic detection techniques should therefore be considered as well.

  14. Geologic exploration of Mars

    NASA Technical Reports Server (NTRS)

    Plescia, J. B.

    1990-01-01

    The scientific objectives and methods involved in a geologic exploration of Mars from a manned outpost are discussed. The constraints on outpost activities imposed by the limited crew size, limited amount of time available for science, the limited diversity of scientific expertise, and the competition between scientific disciplines are addressed. Three examples of possible outpost locations are examined: the Olympus Mons aureole, Mangala Valles/Daedalia Planum, and Candor Chasma. The geologic work that could be done at each site is pointed out.

  15. Postremediation dose assessment for the former Alba Craft Laboratory site, Oxford, Ohio

    SciTech Connect

    Kamboj, S.; Nimmagadda, M.; Yu, C.

    1996-04-01

    Potential maximum radiation dose rates were calculated for the former Alba Craft Laboratory site in Oxford, Ohio, which was involved in machining of uranium metal in the 1950s for the U.S. atomic energy program. The site is not currently being used. The residual radioactive material guidelines (RESRAD) computer code, which implements the methodology described in the US Department of Energy`s (DOE`s) manual for establishing residual radioactive material guidelines, was sued in this evaluation. Three potential land use scenarios were considered for the former Alba Craft site; the scenarios vary with regard to the type of site use, time spent at the site by the exposed individual, and sources of food consumed. Scenario A (a possible land use scenario) assumed industrial use of the site; Scenario B (a likely future land use scenario) assumed residential use of the site; and Scenario C (a possible but unlikely land use scenario) assumed the presence of a resident farmer. For scenario A, it was assumed that any water used for domestic or industrial activities would be from uncontaminated off-site municipal sources. The water used for drinking, household purposes, and irrigation was assumed to be from uncontaminated municipal sources in Scenario B; groundwater drawn from a well located at the downgradient edge of the contaminated zone would be the only source of water for drinking, irrigation, and raising livestock in Scenario C. The results of the evaluation indicated that the DOE dose limit of 100 mrem/yr would not be exceeded for any of the scenarios analyzed. The potential maximum dose rates for Scenarios A, B, and C are 0.64, 2.0, and 11 mrem/yr, respectively.

  16. Mars on Earth: soil analogues for future Mars missions

    NASA Astrophysics Data System (ADS)

    Marlow, Jeffrey J.; Martins, Zita; Sephton, Mark A.

    2008-04-01

    Preparations for missions to Mars are a major concern for scientists. Predicting how equipment and experiments will perform on the planet is difficult because tests are restricted to Earth. Mars soil analogues are being used to solve this problem. These terrestrial materials are chemically and physically similar to martian soils and, because they contain unusual minerals and trace amounts of organic matter, are scientifically interesting in their own right. However, no current analogue is appropriate for all necessary tests. Here we describe Mars soil analogues, identify limitations and suggest the need for new Mars simulants.

  17. Making Mars habitable

    NASA Astrophysics Data System (ADS)

    McKay, Christopher P.; Toon, Owen B.; Kasting, James F.

    1991-08-01

    The possibility is considered that the atmosphere and climate of Mars could be altered to allow terrestrial life forms, and possibly human beings, to survive on the surface. Production of CFCs or other greenhouse gases on Mars would warm the surface enough for the regolith and polar caps to release their CO2 and raise atmospheric pressure to 100 mbar. If a large regolith and polar CO2 reservoirs exist, the pressure would continue to rise on its own. If these are absent, additional CO2 would have to be released from carbonate minerals. At this point, perhaps between 100 and 100,000 yrs, Mars might be suitable for plants. If there is a mechanism for sequestering the reduced carbon, these plants could slowly transform the CO2 to produce an O2-rich atmosphere in perhaps 100,000 yrs. If sufficient N2 could be released from putative soil deposits and the CO2 level could be kept low enough, then a human-breathable atmosphere would be produced.

  18. Making Mars habitable

    NASA Technical Reports Server (NTRS)

    Mckay, Christopher P.; Toon, Owen B.; Kasting, James F.

    1991-01-01

    The possibility is considered that the atmosphere and climate of Mars could be altered to allow terrestrial life forms, and possibly human beings, to survive on the surface. Production of CFCs or other greenhouse gases on Mars would warm the surface enough for the regolith and polar caps to release their CO2 and raise atmospheric pressure to 100 mbar. If a large regolith and polar CO2 reservoirs exist, the pressure would continue to rise on its own. If these are absent, additional CO2 would have to be released from carbonate minerals. At this point, perhaps between 100 and 100,000 yrs, Mars might be suitable for plants. If there is a mechanism for sequestering the reduced carbon, these plants could slowly transform the CO2 to produce an O2-rich atmosphere in perhaps 100,000 yrs. If sufficient N2 could be released from putative soil deposits and the CO2 level could be kept low enough, then a human-breathable atmosphere would be produced.

  19. Abiogenic synthesis on Mars.

    PubMed

    Young, R S; Ponnamperuma, C; McCaw, B K

    1965-01-01

    Atmospheres capable of producing organic compounds under primitive conditions are discussed in the light of recent experimental evidence. The atmosphere of Mars is discussed, in particular, the observations of Sinton of reflection spectra with features at 3.45, 3.58, and 3.69, which are attributes to C-H bands and the presence of organic molecules. Colthup interprets these features as being representative of organic aldehydes and suggests specifically, acetaldehyde. Many works have considered these observations as being indicative of life on Mars. Rea has offered alternative hypotheses. This paper presents experimental evidence of yet another possible explanation; that organic compounds are being produced in the Martian atmosphere, and may be responsible for Sinton's observations. The influence of such syntheses on possible Martian organisms is discussed. Various possible Martian atmospheres have been irradiated with ultraviolet light as well as other possible energy sources and a variety of organic end products have been identified. Martian atmospheres plus acetaldehyde as a starting point have also been used and end products analyzed. Possible abiogenic pathways for Mars are discussed.

  20. On Target to Mars

    NASA Technical Reports Server (NTRS)

    Cheng, Yang

    2007-01-01

    This viewgraph presentation reviews the use of Descent Image Motion Estimation System (DIMES) for the descent of a spacecraft onto the surface of Mars. In the past this system was used to assist in the landing of the MER spacecraft. The overall algorithm is reviewed, and views of the hardware, and views from Spirit's descent are shown. On Spirit, had DIMES not been used, the impact velocity would have been at the limit of the airbag capability and Spirit may have bounced into Endurance Crater. By using DIMES, the velocity was reduced to well within the bounds of the airbag performance and Spirit arrived safely at Mars. Views from Oppurtunity's descent are also shown. The system to avoid and detect hazards is reviewed next. Landmark Based Spacecraft Pinpoint Landing is also reviewed. A cartoon version of a pinpoint landing and the various points is shown. Mars s surface has a large amount of craters, which are ideal landmarks . According to literatures on Martian cratering, 60 % of Martian surface is heavily cratered. The ideal (craters) landmarks for pinpoint landing will be between 1000 to 50 meters in diagonal The ideal altitude for position estimation should greater than 2 km above the ground. The algorithms used to detect and match craters are reviewed.

  1. Benzene Production on Mars

    NASA Astrophysics Data System (ADS)

    Muscatello, Anthony C.; Berggren, Mark H.; Strott, David K.; Zubrin, Robert M.

    2004-02-01

    The Methane to Aromatics on Mars (METAMARS) system is an in situ resource utilization (ISRU) technique that converts methane produced from the carbon dioxide in the martian atmosphere to low hydrogen content liquid aromatic fuels for an Earth Return Vehicle, thus greatly increasing the leverage of the hydrogen imported from the Earth. More importantly, the METAMARS system reduces the amount of hydrogen imported from Earth by a factor of four, leading to dramatic reductions in mission cost. This project involves design and construction of two fully functional oxygen/aromatic hydrocarbon production facilities (brassboard and protoflight) sized to produce 1 kg of bipropellant per day. Because aromatic fuels contain only about one hydrogen atom per carbon atom, the METAMARS system gives extremely high leverages on the order of 53 in the production of fuel and oxidizer for a Mars Sample Return (MSR) mission and human Mars missions. In addition, there are extensive potential commercial applications for the technology in converting trillions of cubic feet of stranded natural gas into easily transportable liquid aromatic products.

  2. Mars Observer camera

    NASA Technical Reports Server (NTRS)

    Malin, M. C.; Danielson, G. E.; Ingersoll, A. P.; Masursky, H.; Veverka, J.; Ravine, M. A.; Soulanille, T. A.

    1992-01-01

    The Mars Observer camera (MOC) is a three-component system (one narrow-angle and two wide-angle cameras) designed to take high spatial resolution pictures of the surface of Mars and to obtain lower spatial resolution, synoptic coverage of the planet's surface and atmosphere. The cameras are based on the 'push broom' technique; that is, they do not take 'frames' but rather build pictures, one line at a time, as the spacecraft moves around the planet in its orbit. MOC is primarily a telescope for taking extremely high resolution pictures of selected locations on Mars. Using the narrow-angle camera, areas ranging from 2.8 km x 2.8 km to 2.8 km x 25.2 km (depending on available internal digital buffer memory) can be photographed at about 1.4 m/pixel. Additionally, lower-resolution pictures (to a lowest resolution of about 11 m/pixel) can be acquired by pixel averaging; these images can be much longer, ranging up to 2.8 x 500 km at 11 m/pixel. High-resolution data will be used to study sediments and sedimentary processes, polar processes and deposits, volcanism, and other geologic/geomorphic processes.

  3. Sustainable Mars Sample Return

    NASA Technical Reports Server (NTRS)

    Alston, Christie; Hancock, Sean; Laub, Joshua; Perry, Christopher; Ash, Robert

    2011-01-01

    The proposed Mars sample return mission will be completed using natural Martian resources for the majority of its operations. The system uses the following technologies: In-Situ Propellant Production (ISPP), a methane-oxygen propelled Mars Ascent Vehicle (MAV), a carbon dioxide powered hopper, and a hydrogen fueled balloon system (large balloons and small weather balloons). The ISPP system will produce the hydrogen, methane, and oxygen using a Sabatier reactor. a water electrolysis cell, water extracted from the Martian surface, and carbon dioxide extracted from the Martian atmosphere. Indigenous hydrogen will fuel the balloon systems and locally-derived methane and oxygen will fuel the MAV for the return of a 50 kg sample to Earth. The ISPP system will have a production cycle of 800 days and the estimated overall mission length is 1355 days from Earth departure to return to low Earth orbit. Combining these advanced technologies will enable the proposed sample return mission to be executed with reduced initial launch mass and thus be more cost efficient. The successful completion of this mission will serve as the next step in the advancement of Mars exploration technology.

  4. Mars Rocket Propulsion System

    NASA Technical Reports Server (NTRS)

    Zubrin, Robert; Harber, Dan; Nabors, Sammy

    2008-01-01

    A report discusses the methane and carbon monoxide/LOX (McLOx) rocket for ascent from Mars as well as other critical space propulsion tasks. The system offers a specific impulse over 370 s roughly 50 s higher than existing space-storable bio-propellants. Current Mars in-situ propellant production (ISPP) technologies produce impure methane and carbon monoxide in various combinations. While separation and purification of methane fuel is possible, it adds complexity to the propellant production process and discards an otherwise useful fuel product. The McLOx makes such complex and wasteful processes unnecessary by burning the methane/CO mixtures produced by the Mars ISPP systems without the need for further refinement. Despite the decrease in rocket-specific impulse caused by the CO admixture, the improvement offered by concomitant increased propellant density can provide a net improvement in stage performance. One advantage is the increase of the total amount of propellant produced, but with a decrease in mass and complexity of the required ISPP plant. Methane/CO fuel mixtures also may be produced by reprocessing the organic wastes of a Moon base or a space station, making McLOx engines key for a human Lunar initiative or the International Space Station (ISS) program. Because McLOx propellant components store at a common temperature, very lightweight and compact common bulkhead tanks can be employed, improving overall stage performance further.

  5. Exobiological exploration of Mars.

    PubMed

    Klein, H P; DeVincenzi, D L

    1995-03-01

    Of all the other planets in the solar system, Mars remains the most promising for further elucidating concepts about chemical evolution and the origin of life. Strategies were developed to pursue three exobiological objectives for Mars exploration: determining the abundance and distribution of the biogenic elements and organic compounds, detecting evidence of an ancient biota on Mars, and determining whether indigenous organisms exist anywhere on the planet. The three strategies are quite similar and, in fact, share the same sequence of phases. In the first phase, each requires global reconnaissance and remote sensing by orbiters to select sites of interest for detailed in situ analyses. In the second phase, lander missions are conducted to characterize the chemical and physical properties of the selected sites. The third phase involves conducting "critical" experiments at sites whose properties make them particularly attractive for exobiology. These critical experiments would include, for example, identification of organics, detection of fossils, and detection of extant life. The fourth phase is the detailed analysis of samples returned from these sites in Earth-based laboratories to confirm and extend previous discoveries. Finally, in the fifth phase, human exploration is needed to establish the geological settings for the earlier findings or to discover and explore sites that are not accessible to robotic spacecraft.

  6. Electrical power systems for Mars

    NASA Technical Reports Server (NTRS)

    Giudici, Robert J.

    1986-01-01

    Electrical power system options for Mars Manned Modules and Mars Surface Bases were evaluated for both near-term and advanced performance potential. The power system options investigated for the Mission Modules include photovoltaics, solar thermal, nuclear reactor, and isotope power systems. Options discussed for Mars Bases include the above options with the addition of a brief discussion of open loop energy conversion of Mars resources, including utilization of wind, subsurface thermal gradients, and super oxides. Electrical power requirements for Mission Modules were estimated for three basic approaches: as a function of crew size; as a function of electric propulsion; and as a function of transmission of power from an orbiter to the surface of Mars via laser or radio frequency. Mars Base power requirements were assumed to be determined by production facilities that make resources available for follow-on missions leading to the establishment of a permanently manned Base. Requirements include the production of buffer gas and propellant production plants.

  7. Electrical power systems for Mars

    NASA Astrophysics Data System (ADS)

    Giudici, Robert J.

    1986-05-01

    Electrical power system options for Mars Manned Modules and Mars Surface Bases were evaluated for both near-term and advanced performance potential. The power system options investigated for the Mission Modules include photovoltaics, solar thermal, nuclear reactor, and isotope power systems. Options discussed for Mars Bases include the above options with the addition of a brief discussion of open loop energy conversion of Mars resources, including utilization of wind, subsurface thermal gradients, and super oxides. Electrical power requirements for Mission Modules were estimated for three basic approaches: as a function of crew size; as a function of electric propulsion; and as a function of transmission of power from an orbiter to the surface of Mars via laser or radio frequency. Mars Base power requirements were assumed to be determined by production facilities that make resources available for follow-on missions leading to the establishment of a permanently manned Base. Requirements include the production of buffer gas and propellant production plants.

  8. Mars solar conjunction prediction modeling

    NASA Astrophysics Data System (ADS)

    Srivastava, Vineet K.; Kumar, Jai; Kulshrestha, Shivali; Kushvah, Badam Singh

    2016-01-01

    During the Mars solar conjunction, telecommunication and tracking between the spacecraft and the Earth degrades significantly. The radio signal degradation depends on the angular separation between the Sun, Earth and probe (SEP), the signal frequency band and the solar activity. All radiometric tracking data types display increased noise and signatures for smaller SEP angles. Due to scintillation, telemetry frame errors increase significantly when solar elongation becomes small enough. This degradation in telemetry data return starts at solar elongation angles of around 5° at S-band, around 2° at X-band and about 1° at Ka-band. This paper presents a mathematical model for predicting Mars superior solar conjunction for any Mars orbiting spacecraft. The described model is simulated for the Mars Orbiter Mission which experienced Mars solar conjunction during May-July 2015. Such a model may be useful to flight projects and design engineers in the planning of Mars solar conjunction operational scenarios.

  9. Workshop on Mars Telescopic Observations

    NASA Technical Reports Server (NTRS)

    Bell, J. F., III (Editor); Moersch, J. E. (Editor)

    1995-01-01

    The Mars Telescopic Observations Workshop, held August 14-15, 1995, at Cornell University in Ithaca, New York, was organized and planned with two primary goals in mind: The first goal was to facilitate discussions among and between amateur and professional observers and to create a workshop environment fostering collaborations and comparisons within the Mars observing community. The second goal was to explore the role of continuing telescopic observations of Mars in the upcoming era of increased spacecraft exploration. The 24 papers presented at the workshop described the current NASA plans for Mars exploration over the next decade, current and recent Mars research being performed by professional astronomers, and current and past Mars observations being performed by amateur observers and observing associations. The workshop was divided into short topical sessions concentrating on programmatic overviews, groundbased support of upcoming spacecraft experiments, atmospheric observations, surface observations, modeling and numerical studies, and contributions from amateur astronomers.

  10. Mars periglacial punctual features analyses

    NASA Astrophysics Data System (ADS)

    Machado, Adriane; Barata, Teresa; Ivo Alves, E.; Cunha, Pedro P.

    2012-11-01

    The presence of patterned grounds on Mars has been reported in several papers, especially the study of polygons distribution, size and formation processes. In the last years, the presence of basketball terrains has been noticed on Mars. Studies were made to recognize these terrains on Mars through the analysis of Mars Orbiter Camera (MOC) images. We have been developing an algorithm that recognizes automatically and extracts the hummocky patterns on Mars related to landforms generated by freeze-thaw cycles such as mud boils features. The algorithm is based on remote sensing data that establishes a comparison between the hummocks and mud boils morphology and size from Adventdalen at Longyearbyen (Svalbard - Norway) and hummocky patterns on Mars using High Resolution Imaging Science Experiment (HiRISE) imagery.

  11. Measuring Mars Sand Flux Seasonality from a Time Series of Hirise Images

    NASA Astrophysics Data System (ADS)

    Ayoub, F.; Avouac, J.; Bridges, N. T.; Leprince, S.; Lucas, A.

    2012-12-01

    The volumetric transport rate of sand, or flux, is a fundamental quantity that relates to the rate of landscape evolution through surface deposition and erosion. Measuring this quantity on Mars is particularly relevant as wind is the dominant geomorphic agent active at present on the planet. Measuring sand flux on Mars has been made possible thanks to the availability of times series of high resolution images acquired by the High Resolution Imaging Science Experiment (HiRISE) and precise image registration and correlation methods which permits the quantification of movement to sub-pixel precision. In this study, focused on the Nili Patera dune field, we first measured the migration rate of sand ripples and dune lee fronts over 105 days, using a pair of HiRISE images acquired in 2007, correlated and co-registered with COSI-Corr. From these measurements and the estimation of the ripple and dune heights, we derived the reptation and saltation sand fluxes. We next applied the same methodology to a time-series of eight images acquired in 2010-2011 covering one Mars year. Pairs of sequential images, were processed with COSI-Corr yielding a times series of 8 displacement maps. A Principal Component Analysis (PCA) was applied to the time-series to quantify more robustly the time evolution of the signal and filter out noise, in particular due to misalignment of CCDs. Using the first two components, which account for 84% of the variance, the seasonal variation of the ripple migration rate was estimated. We clearly observe continuously active migration throughout the year with a strong seasonal quasi-sinusoidal variation which peaks at perihelion. Ripple displacement orientation is stable in time, toward ~N115°E. The wind direction is thus relatively constant in this area, a finding consistent with the barchan morphology and orientation of the dunes. The dataset require that sand moving winds must occur daily to weekly throughout the year. The amplitude of the seasonal

  12. Origin and evolution of valleys on Martian volcanoes

    SciTech Connect

    Gulick, V.C.; Baker, V.R. )

    1990-08-30

    Morphological analyses of six Martian volcanoes, Ceraunius Tholus, Hecates Tholus, Alba Patera, Hadriaca Patera, Apollinaris Patera, and Tyrrhena Patera, indicate that fluvial processes were the dominant influence in the initiation and subsequent development of many dissecting valleys. Lava processes and possibly volcanic density flows were also important as valley-forming processes. Fluvial valleys are especially well developed on Alba Patera, Ceraunius Tholus, and Hecates Tholus. These valleys are inset into the surrounding landscape. They formed in regions of subdued lava flow morphology, contain tributaries, and tend to widen slightly in the downstream direction. Lava channels on Alba Patera are located on the crest of lava flows and have a discontinuous, irregular surface morphology, and distributary patterns. These channels sometimes narrow toward their termini. Possible volcanic density flow channels are located on the northern flank of Ceraunius Tholus. Valleys dissecting Apollinaris Patera, Hadriaca Patera, and Tyrrhena Patera appear to have a complex evolution, probably a mixed fluvial and lava origin. They are inset into a subdued (possibly mantled) surface, lack tributaries, and either have fairly constant widths or widen slightly downvalley. Valleys surrounding the caldera of Apollinaris appear to have formed by fluvial and possibly by volcanic density flow processes, while those on the Apollinaris fan structure may have a mixed lava and fluvial origin. Valleys on Tyrrhena have broad flat floors and theater heads, which have been extensively enlarged, probably by sapping.

  13. Mars Aqueous Processing System

    NASA Technical Reports Server (NTRS)

    Berggren, Mark; Wilson, Cherie; Carrera, Stacy; Rose, Heather; Muscatello, Anthony; Kilgore, James; Zubrin, Robert

    2012-01-01

    The goal of the Mars Aqueous Processing System (MAPS) is to establish a flexible process that generates multiple products that are useful for human habitation. Selectively extracting useful components into an aqueous solution, and then sequentially recovering individual constituents, can obtain a suite of refined or semi-refined products. Similarities in the bulk composition (although not necessarily of the mineralogy) of Martian and Lunar soils potentially make MAPS widely applicable. Similar process steps can be conducted on both Mars and Lunar soils while tailoring the reaction extents and recoveries to the specifics of each location. The MAPS closed-loop process selectively extracts, and then recovers, constituents from soils using acids and bases. The emphasis on Mars involves the production of useful materials such as iron, silica, alumina, magnesia, and concrete with recovery of oxygen as a byproduct. On the Moon, similar chemistry is applied with emphasis on oxygen production. This innovation has been demonstrated to produce high-grade materials, such as metallic iron, aluminum oxide, magnesium oxide, and calcium oxide, from lunar and Martian soil simulants. Most of the target products exhibited purities of 80 to 90 percent or more, allowing direct use for many potential applications. Up to one-fourth of the feed soil mass was converted to metal, metal oxide, and oxygen products. The soil residue contained elevated silica content, allowing for potential additional refining and extraction for recovery of materials needed for photovoltaic, semiconductor, and glass applications. A high-grade iron oxide concentrate derived from lunar soil simulant was used to produce a metallic iron component using a novel, combined hydrogen reduction/metal sintering technique. The part was subsequently machined and found to be structurally sound. The behavior of the lunar-simulant-derived iron product was very similar to that produced using the same methods on a Michigan iron

  14. Global View of Mars Topography

    NASA Technical Reports Server (NTRS)

    2007-01-01

    [figure removed for brevity, see original site] Annotated Version

    This global map of Mars is based on topographical information collected by the Mars Orbiter Laser Altimeter instrument on NASA's Mars Global Surveyor orbiter. Illumination is from the upper right. The image width is approximately 18,000 kilometers (11,185 miles). Candor Chasma forms part of the large Martian canyon system named Valles Marineris. The location of Southwest Candor Chasma is indicated in the annotated version.

  15. Antidepressant-like effects of the ethyl acetate soluble fraction of the root bark of Morus alba on the immobility behavior of rats in the forced swim test.

    PubMed

    Lim, Dong Wook; Kim, Yun Tai; Park, Ji-Hae; Baek, Nam-In; Han, Daeseok

    2014-06-12

    In this study, the antidepressant-like effects of Morus alba fractions in rats were investigated in the forced swim test (FST). Male Wistar rats (9-week-old) were administered orally the M. alba ethyl acetate (EtOAc 30 and 100 mg/kg) and M. alba n-butanol fractions (n-BuOH 30 and 100 mg/kg) every day for 7 consecutive days. On day 7, 1 h after the final administration of the fractions, the rats were exposed to the FST. M. alba EtOAc fraction at the dose of 100 mg/kg induced a decrease in immobility behavior (p < 0.01) with a concomitant increase in both climbing (p < 0.05) and swimming (p < 0.05) behaviors when compared with the control group, and M. alba EtOAc fraction at the dose of 100 mg/kg decreased the hypothalamic-pituitary-adrenal (HPA) axis response to the stress, as indicated by an attenuated corticosterone response and decreased c-fos immunoreactivity in the hippocampal and hypothalamic paraventricular nucleus (PVN) region. These findings demonstrated that M. alba EtOAc fraction have beneficial effects on depressive behaviors and restore both altered c-fos expression and HPA activity.

  16. Mars gravity and climate

    NASA Astrophysics Data System (ADS)

    Bills, B. G.; Mischna, M. A.

    2011-12-01

    How accurately do we need to measure seasonal variations in Mars gravity, in order to significantly contribute to an understanding of the seasonal climate cycle? It has long been understood that seasonal cycles of volatile mass transport on Mars, mainly involving CO2 exchange between the atmosphere and the polar caps, will change the gravitational field by measurable amounts. In recent years, the gravitational field models, which are obtained from measured Doppler shifts in the tracking data for Mars-orbiting satellites, have become accurate enough that they can resolve some seasonal variations. However, the present models only resolve seasonal cycles for two parameters, nominally J2 and J3, which are zonal components of degree 2 and 3, respectively. In fact, what is actually observed is an unresolved linear combination of even degree zonals, in the guise of J2, and a similar combination of odd degree zonals for J3. Mars climate models are currently constrained mainly by the surface atmospheric pressure measurements made at the two Viking Lander sites. Wood and Paige (1992) showed that the observed seasonal pressure cycles at these two locations can be very well simulated by a simple one-dimensional surface thermal balance model, when its 6 free parameters (separate values for albedo and emissivity for each polar cap, and a soil thermal inertia for each hemisphere ) are properly chosen. However, it also emerged that the preferred values for albedo and emissivity are quite different from those obtained via optical remote sensing. It thus appears that the 1-D climate model yields aliased estimates of these parameters. It seems clear that, if we had sufficiently accurate gravity measurements, it would be equivalent to having a global grid of effective Viking Lander pressure measurements, with the number of grid points related to the spatial resolution of the gravity measurements. For example, if the seasonal variations were seen in a full Nth degree and order gravity

  17. The investigation of moving dunes over Mars using very high resolution topography and sub pixel co-registration method.

    NASA Astrophysics Data System (ADS)

    Kim, J.; Baik, H.; Seol, H.

    2015-12-01

    Although the origins and processes of Martian aeolian features, especially dunes, have not been fully identified yet, it has been better understood by the orbital observation method which has led to the identification of Martian dune migration such as a case in Nili Patera (Bridges, 2012), and the numerical model employing advanced computational fluid dynamics. Specifically, the recent introduction of very high-resolution image products, such as 25 cm-resolution HiRISE imagery and its precise photogrammetric processor, allows us to trace the estimated, although tiny, dune migration over the Martian surface. In this study, we attempted to improve the accuracy of active dune migration measurements by 1) the introduction of very high resolution ortho images and stereo analysis based on the hierarchical geodetic control (Kim and Muller, 2009) for better initial point settings; and 2) the improved sub-pixel co-registration algorithms using optical flow with a refinement stage based on a least squares correlation conducted on a pyramidal processor. Consequently, this scheme not only measured Martian dune migration more precisely, but it also achieved the extension of 3D observations combining stereo analysis and photoclinometry. The established algorithms have been tested using the HiRISE time series images over several dune fields, such as the Kaiser, Procter, and Rabe craters, which were reported by the Mars Global Digital Dune Database (Hayward et al., 2013). The detected dune migrations were significantly larger than previously reported values. The outcomes in our study will be demonstrated with the quantified values in 2D and volumetric direction. In the future, the method will be further applied to the dune fields in the Mars Global dune database comprehensively and can be compared with the improved General Circulation Model and the numerical simulation.

  18. Instrument Deployment for Mars Rovers

    NASA Technical Reports Server (NTRS)

    Pedersen, Liam; Bualat, Maria; Kunz, C.; Lee, Susan; Sargent, Randy; Washington, Rich; Wright, Anne; Clancy, Daniel (Technical Monitor)

    2002-01-01

    Future Mars rovers, such as the planned 2009 MSL rover, require sufficient autonomy to robustly approach rock targets and place an instrument in contact with them. It took the 1997 Sojourner Mars rover between 3 and 5 communications cycles to accomplish this. This paper describes the technologies being developed and integrated onto the NASA Ames K9 prototype Mars rover to both accomplish this in one cycle, and to extend the complexity and duration of operations that a Mars rover can accomplish without intervention from mission control.

  19. Hot oxygen corona of Mars

    SciTech Connect

    Ip, W.H.

    1988-10-01

    Electron dissociative recombination of O2(+) ions in the Venus ionosphere, which may be an important source of suprathermal atomic oxygen, is presently considered as a factor in the Mars exosphere; due to the weaker surface gravitational attraction of Mars, a hot oxygen corona thus formed would be denser than that of Venus at altitudes greater than 2000 km despite Mars' lower ionospheric content. If such an extended oxygen corona does exist on Mars, its collisional interaction with Phobos would lead to the formation of an oxygen gas torus whose average number density is of the order of only 1-2/cu cm along the Phobos orbit. 51 references.

  20. Mars gravitational field estimation error

    NASA Technical Reports Server (NTRS)

    Compton, H. R.; Daniels, E. F.

    1972-01-01

    The error covariance matrices associated with a weighted least-squares differential correction process have been analyzed for accuracy in determining the gravitational coefficients through degree and order five in the Mars gravitational potential junction. The results are presented in terms of standard deviations for the assumed estimated parameters. The covariance matrices were calculated by assuming Doppler tracking data from a Mars orbiter, a priori statistics for the estimated parameters, and model error uncertainties for tracking-station locations, the Mars ephemeris, the astronomical unit, the Mars gravitational constant (G sub M), and the gravitational coefficients of degrees six and seven. Model errors were treated by using the concept of consider parameters.