nasa scientific and technical aerospace reports phần 7 pps

20050170004 Jet Propulsion Lab., California Inst. of Tech., Pasadena, CA, USA
Elastic Thickness Estimates for Coronae Associated with Chasmata on Venus
Hoogenboom, T.; Martin, P.; Housean, G. A.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also
20050169945; Original contains black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI
on CD-ROM only as part of the entire parent document
Coronae are large-scale circular tectonic features surrounded by annular ridges. They are generally considered unique to
Venus and may offer insights into the differences in lithospheric structure or mantle convective pattern between Venus and
Earth. 68% of all coronae are associated with chasmata or fracture belts. The remaining 32% are located at volcanic rises or
in the plains. Chasmata are linear to arcuate troughs, with trough parallel fractures and faults which extend for 1000 s of
kilometers. Estimates of the elastic thickness of the lithosphere (T(sub e)) have been calculated in a number of
gravity/topography studies of Venus and for coronae specifically. None of these studies, however, have explored the
dependence of T(sub e) on the tectonic history of the region, as implied from the interpretation of relative timing relationships
between coronae and surrounding features. We examine the relationship between the local T(sub e) and the relative ages of
coronae and chasmata with the aim of further constraining the origin and evolution of coronae and chasmata systems.
Derived from text
Coronas; Planetary Geology; Venus (Planet); Tectonics; Thickness; Elastic Properties; Landforms; Topography
20050170005 Los Alamos National Lab., NM, USA
LIBS-based Detection of Geological Samples at Low Pressures (\h0.0001 torr) for Moon and Asteroid Exploration
Harris, R. D.; Cremers, D. A.; Khoo, C.; Benelli, K.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English;
See also 20050169945; Original contains color and black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy;
Available from CASI on CD-ROM only as part of the entire parent document
LIBS is under development for future use on surface probes to Mars [1-3]. Under simulated Mars atmospheric
composition and pressure (7 torr, predominately CO2), LIBS has been shown useful for qualitative and quantitative analysis
of geological samples at close and stand-off distances (19 m). Because of its many advantages compared to previously
deployed and current in-use methods of elemental analysis (e.g. x-ray fluorescence, APXS), LIBS has potential for application
to other planetary bodies. Of particular interest are the Moon and asteroids having very low ambient gas pressures at the
surface. Because the laser plasma used by LIBS is sensitive to the surrounding atmosphere, it is important to determine
analysis capabilities under these conditions. The results of a study of LIBS capabilities at low pressure is presented here for

both in-situ and stand-off analysis. Plasma light, collected through the evacuated tube by a 10 cm diameter quartz lens, was
focused onto a fiber optic cable. The light was directed into either the
Derived from text
Laser-Induced Breakdown Spectroscopy; Mars Atmosphere; Qualitative Analysis; Quantitative Analysis; Geology; Asteroids;
Moon; Atmospheric Composition; Chemical Analysis
20050170006 Collegium Budapest/Inst. for Advanced Study, Budapest, Hungary
Annual Change of Martian DDS-Seepages
Horvaith, A.; Kereszturi, A.; Berezi, Sz.; Sik, A.; Pocs, T.; Gesztesi, A.; Ganti, T.; Szathmary, E.; Lunar and Planetary Science
XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color and black and white illustrations;
Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
The signs of surface water found by MGS (on MOC images), Mars Odyssey (neutron data) and Mars Express (spectral
data) play important role in understanding surface processes especially probable life forms on Mars. There are signs of recent
liquid water on Mars like the gullies formed probably during high obliquity and dark slope streaks which could be formed by
gravitational mass movements or water seepage. We discovered and analysed a possible third group of phenomena presumably
produced by liquid water on the surface, called DDS-seepage. These are originated at dark dune spots (DDS). (Dark dune spots
appear in the defrosting surface in late winter early spring in the polar regions of Mars). Most of the DDS-seepages can be
found at the steep slopes of the dark dunes in craters and the intercrater areas and we could study not only great number of
these seepages but also could observe their changes from one Martian year to the other.
Derived from text
Dunes; Seepage; Mars Surface; Extraterrestrial Life; Annual Variations
355
20050170007 Brown Univ., Providence, RI, USA
Regional Mid-Latitude Late Amazonian Valley Glaciers on Mars: Origin of Lineated Valley Fill and Implications for
Recent Climate Change
Head, James W.; Marchant, David r.; Agnew, Marshall C.; Fassett, Caleb I.; Kreslavsky, Mikhail A.; Lunar and Planetary
Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color and black and white
illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent
document

Among the hallmark morphologies of the highland-lowland boundary region in the northern mid-latitude Deuteronilus-
Protonilus Mensae area (30-50oN, 315-350oW) is the fretted terrain (1), consisting of 1) debris aprons that surround many
of the massifs and valley walls, and 2) lineated valley fill (LVF) that occurs on the floors of many of the valleys (2-14). The
ages of these deposits are typically much younger than the adjacent plateau terrain or its breakup and the formation of the
valleys themselves (e.g., 9, 14). The margins of the debris aprons consist of rounded and convex upward topography, and at
Viking resolution the debris aprons and the valley fill can appear smooth and relatively homogeneous or, in contrast, can be
characterized by closely spaced parallel ridges and grooves a few to several tens of meters high. These sets of parallel ridges
have been interpreted to have formed both parallel and normal to valley and mesa walls. Some workers (e.g., 2) argue that
the lineations form mostly normal to flow due to converging flow from debris aprons on opposite sides of valleys or mesas,
while others (e.g., 4) argue that bending of ridges and grooves entering valleys from a side tributary supports flow in the
direction parallel to the valley. Recent analysis shows variable downslope gradients suggesting that lateral flow was minimal
(e.g., 11). All agree that the materials represent some sort of viscous flow processes, but opinions differ on the details of the
mechanism; most authors call on processes of gravity-driven debris flow, assisted by ice or water in the interstices derived
from either groundwater or diffusive exchange with the atmosphere (e.g., see 7, 10, 13-14). Some liken the process to
rock-glacial flow (e.g., 2, 4) with the source of the lubricating agent being ice from atmospheric frost deposition and diffusion
(2) or mobilized interstitial ground ice (4).
Derived from text
Climate Change; Glaciers; Mars Surface; Valleys; Highlands
20050170008 Lunar and Planetary Inst., Houston, TX, USA
Loss Tangent Map of the Martian Surface: A Frequency Dependent Model for the Near Equatorial Regions
Heggy, E.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains
color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire
parent document
The complex dielectric properties of the Martian surface sediments are a key parameter to understand the physical and
geometrical parameters (such as density and roughness) of the Martian surface. In order to give an experimental description
of the electric behavior of the Martian surface we have undertaken laboratory electromagnetic characterization in the
frequency range 1 MHz to 3 GHz of the total set of minerals identified by TES. Volcanic rocks with a well defined mineralogy
and petrology from potential terrestrial analogues sites have also been included in the study. Our primary objective is to
quantify the range of electrical losses that may be encountered by the various Radar sounding and imaging experiments

dedicated to map the physical properties of the Martian surface and subsurface searching mainly for underground water. The
electromagnetic properties of these Mars-like materials are presented as a function of various geophysical parameters, such
as porosity, bulk density and temperature. Using a basaltic Mars-like soil and soil density distribution provided by TES data.
We integrated those measurements to form a primary Loss tangent and complex dielectric map of the Martian surface.
Author
Mars Surface; Planetary Mapping; Surface Roughness; Density Distribution; Dielectric Properties
20050170010 Deutsche Forschungsanstalt fuer Luft- und Raumfahrt, Berlin, Germany
Beyond the Equilibrium Paradigm:Glacial Deposits in the Equatorial Regions of Mars
Helbert, J.; Benkhoff, J.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945
Contract(s)/Grant(s): DFG-BE-1630/2; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as
part of the entire parent document
While Mars has been considered for a long time a dry place except for the early Noachian, this view has changed in recent
years. This started mainly after the MOC imagery showed features like the gullies and morphological features which can be
associated with glacial activity. Now the motion was discussed that at least small amounts of water or ice had been present
in the recent past on Mars. Still, the common notion was that Mars today is a dry place. With the excellent dataset of the
Gamma and Neutron spectrometer (GRS and HEND) on board of Mars Odyssey this view had to be corrected. The instrument
356
detected water abundance of at least 8wt% in the equatorial regions of Mars and this water is found within the first 2m below
the surface, the penetration depth of the instrument.
Author
2001 Mars Odyssey; Equatorial Regions; Mars Surface; Morphology; Penetration; Water
20050170012 Cologne Univ., Germany
3-Dimensional Chemical Analyses of Components in the Carbonaceous Chondrites Acfer 209 (CR) and Allende (CV)
Hezel, D. C.; Palme, H.; Burkhardt, C.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also
20050169945; Original contains black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI
on CD-ROM only as part of the entire parent document
Components of meteorites are 3-dimensional objects, which are usually studied in 2- dimensional thin sections. One
exception are recent tomographic X-ray studies of Allende volumes by [1]. This method has the disadvantage of producing

only BSE-like images without detailed chemical information: We have started to obtain 3-dimensional chemical data sets for
meteoritic volumes. The results are important for a number of reasons: (1) Calculation of accurate chemical bulk compositions
of chondrules and CAIs. Such data are relatively rare, but of particular interest for a variety of important questions, such as
the chondrule - matrix complementarity described by [2]. A precise knowledge of chondrules compositions is crucial for
chondrule forming mechanisms. Another question related to bulk chondrule compositions is the identification of chondrule
precursor components and their origin [3].
Derived from text
Carbonaceous Chondrites; Chemical Analysis; Chemical Composition; Chondrule; Meteoritic Composition; Meteorites
20050170014 Brown Univ., Providence, RI, USA
Rheological Properties of Late-Stage Lava Flows on Ascraeus Mons: New Evidence from HRSC
Hiesinger, H.; Head, J. W., III; Neukum, G., et al.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English;
See also 20050169945; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire
parent document
The Tharsis Montes, Arsia Mons, Pavonis Mons, and Ascraeus Mons, are large volcanic constructs that are part of the
Tharsis rise. The Tharsis rise is commonly interpreted to be the result of a long-lasting large mantle upwelling that constructed
the rise through a combination of uplift and magmatism (plutonism and volcanism). Of particular interest is the construction
of the huge individual edifices, their ages, duration, episodicity, and rheology. Here we report on estimates of the rheological
properties of late-stage lava flows on the eastern flank of Ascraeus Mons, Mars. Additional information is included in the
original extended abstract.
Author (revised)
Rheology; Mars Volcanoes; Lava; Planetary Geology
20050170016 University of Northern Arizona, Flagstaff, AZ, USA
Martian Central Pit Craters
Hillman, E.; Barlow, N. G.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945;
Original contains color illustrations
Contract(s)/Grant(s): NAG5-12510; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part
of the entire parent document
Impact craters containing central pits are rare on the terrestrial planets but common on icy bodies. Mars is the exception

among the terrestrial planets, where central pits are seen on crater floors ( floor pits ) as well as on top of central peaks ( summit
pits ). Wood et al. [1] proposed that degassing of subsurface volatiles during crater formation produced central pits. Croft [2]
argued instead that central pits might form during the impact of volatile-rich comets. Although central pits are seen in impact
craters on icy moons such as Ganymede, they do show some significant differences from their martian counterparts: (a) only
floor pits are seen on Ganymede, and (b) central pits begin to occur at crater diameters where the peak ring interior
morphology begins to appear in terrestrial planet craters [3]. A study of craters containing central pits was conducted by
Barlow and Bradley [4] using Viking imagery. They found that 28% of craters displaying an interior morphology on Mars
contain central pits. Diameters of craters containing central pits ranged from 16 to 64 km. Barlow and Bradley noted that
summit pit craters tended to be smaller than craters containing floor pits. They also noted a correlation of central pit craters
with the proposed rings of large impact basins. They argued that basin ring formation fractured the martian crust and allowed
subsurface volatiles to concentrate in these locations. They favored the model that degassing of the substrate during crater
357
formation was responsible for central pit formation due to the preferential location of central pit craters along these basin rings.
Derived from text
Mars Craters; Planetary Crusts; Planetary Geology; Structural Basins; Cratering; Mars Surface
20050170017 NASA Ames Research Center, Moffett Field, CA, USA, Virginia Univ., Charlottesville, VA, USA
A Sedimentary Platform in Margaritifer Sinus, Meridiani Terra, and Arabia?
Howard, A. D.; Moore, J. M.; Irwin, R. P., III; Craddock, R. A.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.;
In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available
from CASI on CD-ROM only as part of the entire parent document
The Margaritifer-Meridiani-Arabia highlands-lowlands (H-L) transition has long been recognized as the most fluvially
dissected region of Mars. However, the geomorphic evolution of this region remains enigmatic, particularly the origin of the
layered deposits of Meridiani Terra and Arabia. We suggest that a portion of this regional slope served as a fluvial depositional
platform during the late Noachian.
Derived from text
Geomorphology; Mars Surface; Geochronology; Sediments
20050170018 NASA Johnson Space Center, Houston, TX, USA, National High Magnetic Field Lab., Tallahassee, FL, USA
A Model for Siderophile Element Distribution in Planetary Differentiation
Humayun, M.; Rushmer, T.; Rankenburg, K.; Brandon, A. D.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.;

In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available
from CASI on CD-ROM only as part of the entire parent document
Planetary differentiation begins with partial melting of small planetesimals.At low degrees of partial melting, a sulfur-rich
liquid segregates by physical mechanisms including deformation-assisted porous flow. Experimental studies of the physical
mechanisms by which Fe-S melts segregate from the silicate matrix of a molten H chondrite are part of a companion paper.
Geochemical studies of these experimental products revealed that metallic liquids were in equilibrium with residual metal in
the H chondrite matrix. This contribution explores the geochemical signatures produced by early stages of core formation.
Particularly, low-degree partial melt segregation of Fe-S liquids leaves residual metal in the silicate matrix. Some achondrites
appear to be residues of partial melting, e.g., ureilites, which are known to contain metal. The metal in these achondrites may
show a distinct elemental signature. To quantify the effect of sulfur on siderophile element contents of residual metal we have
developed a model based on recent parametrizations of equilibrium solid metal-liquid metal partitioning experiments.
Derived from text
Protoplanets; Siderophile Elements; Models; Geochemistry
20050170019 State Univ. of New York, Stony Brook, NY, USA
Experimental Basalt Alteration at Low-pH: Implications for Weathering Relationships on Mars
Hurowitz, J. A.; Tosca, N. J.; McLennan, S. M.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See
also 20050169945; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire
parent document
The chemistry of sedimentary rocks has long been utilized for the reconstruction of climatic, geographic and tectonic
conditions in the Earth’s past. Naturally, the chemical and mineralogical changes that accompany weathering of the Earth’s
granodioritic upper crust have been studied in great detail to better understand processes controlling the composition of
sedimentary rocks. Weathering of basaltic rocks has been studied as well, and there is a reasonable understanding of the bulk
chemical and mineralogical changes that accompany alteration of such rocks under terrestrial conditions. In contrast, Martian
soils and altered rocks, which undoubtedly reflect the end product of some combination of physical and/or chemical alteration,
do not appear to have evolved in a manner consistent with alteration of basalts as we know it on Earth. Here we present new
insights into weathering processes on Mars utilizing the results of alteration experiments performed at low pH on synthetic
basalts of Martian composition.
Derived from text

Basalt; Mineralogy; Planetary Geology; pH; Weathering; Mars Surface; Chemical Composition; Sedimentary Rocks
358
20050170021 Idaho State Univ., Pocatello, ID, USA
Petrologic Evidence for Multiple, Chemically Evolved Magma Batches and Implications for Plains Volcanism on Earth
and Mars
Hughes, S. S.; Sakimoto, S. E. H.; Gregg, T. K. P.; Brady, S. M.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.;
In English; See also 20050169945; Original contains color and black and white illustrations; Copyright; Avail: CASI;
A01,
Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
Small mafic shield volcanoes, abundant on the terrestrial planets, are the dominant landform in provinces characterized
by plains-style volcanism. Exemplified on Earth within both oceanic and continental settings (e.g., Hawaii, Snake River
Plains), they provide analogs for similar systems on other planets, especially Mars. Topographic analysis of individual
Quaternary mafic shields on the eastern Snake River Plains (ESRP) of Idaho (the type area for plains-style volcanism
demonstrates similarity in size, volume, and shape of these shields, as well as the vent spacing in the volcanic fields, with those
of the Tempe Terra and Syria Planum regions of Mars. Geochemical and physical volcanologic studies of the ESRP show an
emerging model of volcanic evolution that implies multiple small batches of magma derived from upper mantle sources.
Various chemical trends are illustrated, exemplified by La vs. MgO, that argue for a system with variably evolved magma
batches and possibly several magmatic sources. Petrologic modeling suggests that early magmas in the sequence form
(layered?) sub-volcanic mafic intrusions that fractionate to evolved compositions. Later mafic magmas commingle with these
earlier-derived intrusions, partially melt and assimilate late-stage fractionates, and erupt with chemically evolved, but
isotopically un-evolved compositions.
Derived from text
Mars Volcanoes; Earth Surface; Petrology; Magma; Plains; Geochemistry; Mineralogy
20050170023 Deutsche Forschungsanstalt fuer Luft- und Raumfahrt, Berlin, Germany
MERTIS: A Thermal Infrared Imaging Spectrometer for the Bepi-Colombo Mission
Helbert, J.; Jessberger, E.; Benkhoff, J.; Arnold, G.; Banaszkiewicz, M.; Bischoff, A.; Blecka, M.; Calcutt, S.; Colangeli, L.,
et al.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
Among the terrestrial planets, Mercury plays a special role. It is the smallest planet, the densest, the one with the probably
oldest surface heavily gardened by space weathering, and shows large daily surface temperature variations. Understanding

Mercury is crucial to develop a better understanding of the early processes in the inner solar system, of how our Earth formed,
how it evolved, and how it interacts with the Sun. The ESA mission Bepi-Colombo consists of two probes - a planetary and
a magnetospheric orbiter. The mission will be launched in 2012 and will reach Mercury in 2016. MERTIS is part of the
payload of the planetary orbiter, focused on understanding the surface and interior of Mercury.
Author
Mercury Surface; Imaging Spectrometers; Thermal Mapping; Surface Temperature
20050170024 Institute of Space and Astronautical Science, Sagamihara, Japan
Formation Process of Lunar Sinuous Rilles by Thermal Erosion of Basaltic Lava Flow
Honda, Chikatoshi; Fujimura, Akio; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also
20050169945; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent
document
One of the major negative relief features on the terrestrial planets and satellites are sinuous rilles, which origin has been
still debated. They possess conspicuous morphological characteristics of meandering channels or valleys, which is decreasing
of depth and width. Normal rilles are straight or gently curved and considered to be graben-type faults. Crater chains in
sometimes form irregular fractures like a rille, but they are excluded from the definition of sinuous rille. Lunar sinuous rilles
are occasionally found in the maria and mare-highland boundaries, and most of them are concentrated around the Mare
Imbrium and in the Oceanus Procellarum. According to, lunar sinuous rilles have typical dimensions of 30 - 40 km length and
of less than 1 km width. The origin of these features differs on each planet or satellite; hence, we investigated the origin of
the lunar sinuous rille due to existence of information for consideration of the origin (e.g., chemical composition of rock and
elevation of rim and floor of sinuous rille).
Derived from text
Lunar Maria; Lunar Topography; Basalt; Lava; Fluid Flow
359
20050170026 Maryland Univ., College Park, MD, USA
Re-187 Os-187 Isotopic and Highly Siderophile Element Systematics of Group IVB Irons
Honesto, J.; McDonough, W. F.; Walker, R. J.; McCoy, T. J.; Ash, R. D.; Lunar and Planetary Science XXXVI, Part 8; [2005];
2 pp.; In English; See also 20050169945; Original contains color illustrations
Contract(s)/Grant(s): NNG04GG17G; NNG04GK52G; NAG5-13464; Copyright; Avail: CASI;
A01, Hardcopy; Available

from CASI on CD-ROM only as part of the entire parent document
Study of the magmatic iron meteorite groups permits constraints to be placed on the chemical and isotopic composition
of parent bodies, and the timing of, and crystal-liquid fractionation processes involved in the crystallization of asteroidal cores.
Here we examine Re-Os isotopic and trace elemental systematics of group IVB irons. Compared to most irons, the irons
comprising this group are enriched in some of the most refractory siderophile elements, yet highly-depleted in most volatile
siderophile elements. These characteristics have been attributed to processes such as high temperature condensation of
precursor materials and oxidation in the parent body. Most recently it has been suggested that both processes may be involved
in the chemical complexity of the group. Here, high precision isotopic and highly siderophile element (HSE) concentrations
are used to further examine these possible origins, and the crystallization history of the group. In addition, we have begun to
assess the possibility of relating certain ungrouped irons with major groups via multi-element, trace element modeling. In a
companion abstract, the isotopic and trace element systematics of the ungrouped iron Tishomingo are compared with the IVB
irons.
Author
Iron Meteorites; Magnetic Materials; Crystallization; Asteroids; Rhenium Isotopes; Osmium Isotopes
20050170027 California Univ., Los Angeles, CA, USA
MET01210: Another Lunar Mare Meteorite (Regolith Breccia) with Extensive Pyroxene Exsolution, and Not Part of
the YQ Launch Pair
Huber, Heinz; Warren, Paul H.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also
20050169945; Original contains color and black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available
from CASI on CD-ROM only as part of the entire parent document
MET01210 has been classified as a lunar anorthositic breccia. Actually, it is a regolith breccia that contains more mare
basalt than highland matter. The bulk Al2O3 content (microprobe fused-bead analysis in excellent agreement with analyses
of the fusion crust) is 16.7 wt%, and the lithic and mineral clast components in thin section appear to be of mainly mare origin.
From pyroxene mg vs. Ti/(Cr+Ti) zonation trends, the dominant mare component probably was a basalt (or diabase) with
approx. 2.2 wt% TiO2. A highland component is definitely present, however. There are small aphanitic anorthositic impact
melt clasts, and four of the five regolith spheroids identified to date are highly aluminous (24-35 wt% Al2O3). One of these,
only 16 m in diameter, is of HASP composition, with 35 wt% Al2O3 and just 34 wt% SiO2 (Kempa and Papike looked for
and did not find a relationship between spheroid size and frequency of HASP; our observations, most notably for lunaite
QUE93069, consistently find HASP most abundant among the smallest highland spheroids and of course surface area/volume

relationships should favor HASP development in relatively small objects.) The only mare or mainly mare spheroid is notably
high in TiO2, 4.6 wt%, particularly considering that the Al2O3/FeO wt. ratio is 1.51, implying that the high-Ti mare
component has been heavily diluted with highland matter. Additional information is included in the original extended abstract.
Author (revised)
Meteorite Parent Bodies; Lunar Rocks; Lunar Maria; Meteoritic Composition
20050170028 State Univ. of New York, Stony Brook, NY, USA
Mechanically Produced Radical Species at Silicate Surfaces and the Oxidant in Martian Soils
Hurowitz, J. A.; Tosca, N. J.; McLennan, S. M.; Schoonen, M. A. A.; Lunar and Planetary Science XXXVI, Part 8; [2005];
2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy;
Available from CASI on CD-ROM only as part of the entire parent document
The Labeled Release (LR) and Gas Exchange (GEx) experiments onboard the Viking Landers determined that the Martian
soils at Chryse and Utopia Planitia contain unknown inorganic species of a highly oxidizing nature. The LR experiment
demonstrated that the addition of a radioactive (14)C labeled nutrient solution to soil samples resulted in the production of
(14)C labeled CO2 due to the breakdown of the organic species introduced. In the GEx experiments, humidification of a 1
cu cm Martian soil sample resulted in the production of as much as 790 nanomoles of O2 gas. The presence of a highly
oxidizing species in the fine, wind-blown soils on Mars has obvious implications for both the stability of organic species in
the Martian near-surface environment, as well as health implications for future human explorers who may be exposed to
reactive dust particles through inhalation. At present, the nature of the oxidant in the Martian soils remains enigmatic.
360
Explanations for their reactivity have called on both exotic chemical compounds and/or unusual formation processes to
produce oxidants. In the medical literature, specifically that related to silicosis and the toxicity of mineral dusts, it has long
been known that the surfaces of freshly ground quartz particles are characterized by highly reactive radical species generated
by the rupture of bonds during the grinding process. These surface radical species are stable in dry environments (e.g. the
Martian surface) and are capable of producing H2O2 and other Reactive Oxygen Species (ROS) in solution. Here, we extend
the study of the reactivity of freshly ground mineral surfaces to include the silicate minerals most commonly encountered in
basalts and soils at the Martian surface: feldspar, clinopyroxene and olivine. We propose that the oxidizing nature of the
Martian soils can be explained by the presence of such mineral surface radical species and propose mechanisms by which they
might be formed under ambient conditions at the Martian surface. Additional information is included in the original extended
abstract.

Author (revised)
Mars Environment; Planetary Composition; Toxicity; Oxidizers; Silicates; Radicals
20050170029 Arizona Univ., Tucson, AZ, USA
Are Martian Crustal Magnetic Anomalies and Valley Networks Concentrated at Low Paleolatitudes?
Hood, Lon L.; Harrison, Keith P.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also
20050169945; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on
CD-ROM only as part of the entire parent document
A broad spatial correlation between the Mars crustal magnetic field and the distribution of valley networks has previously
been reported. Several possible explanations involving magmatic intrusions, hydrothermal alteration of the adjacent crust, and
surface discharge of water have been suggested. In this paper, we investigate whether the distributions of both magnetic
anomalies and valley networks may have been preferentially concentrated at low paleolatitudes. Such a concentration would
be expected if melting of water ice and snow was a stronger source of surface valley erosion in the tropics and if hydrothermal
alteration of crustal rocks played an important role in producing the unusually strong martian magnetic anomalies.
Author
Magnetic Anomalies; Mars (Planet); Crusts; Intrusion
20050170031 Colorado Univ., Boulder, CO, USA
The Etched Terrain in Arabia Terra, Mars, is Tilted
Hynek, B. M.; Phillips, R. J.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945;
Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part
of the entire parent document
Light-toned bedrock has been observed at the Mars Exploration Rover (MER) Opportunity landing site. These outcrops
are rich in a slew of mineral and textural signatures that suggest likely formation within water, including probable evaporites.
Further, remote sensing data suggest that these outcrops are not a local phenomenon, rather, they are exposed across the entire
hematite-bearing plain and well beyond (over an area \g 3 x 10(exp 5) sq km spanning 20 deg of longitude). Recent results
from the OMEGA instrument on Mars Express show that the etched terrain mapped is rich in sulfates, thus corroborating the
hypothesis that outcrops 100s to \g1000 km from Opportunity are diagenetically related. Moreover, there are potentially
correlative terrains (with similar morphologic, thermal, and mineralogic expressions) up to 5,000 km away; including deposits
within the Valles Marineris, Aram Chaos, and isolated exposures across NW Arabia Terra. We are still trying to understand

the full extent of these deposits but it is becoming increasingly clear that copious amounts of water acted over an enormous
region of Mars. Little is known about the timing of the putative sea and diagenesis of the layers. Because of its sedimentary
and apparent subaqueous origin, the etched terrain was likely emplaced as horizontal to sub-horizontal strata. In this study we
test for horizontality of the etched terrain layers and interpret the results in terms of the geological history of this region of
Mars. Additional information is included in the original extended abstract.
Author (revised)
Mars Surface; Bedrock; Erosion; Floods; Terrain; Planetary Geology; Etching; Weathering
20050170551 Lunar and Planetary Inst., Houston, TX, USA
Lunar and Planetary Science XXXVI, Part II
[2005]; ISSN 1540-7848; In English; Lunar and Planetary Science XXXVI, 14-18 Mar. 2005, Houston, TX, USA; See also
20050170552 - 20050170639
Contract(s)/Grant(s): NCC5-679
Report No.(s): LPI-Contrib-1234-Pt-11; Copyright; Avail: CASI;
C01, CD-ROM
361
Some topics covered: Implications of internal fragmentation on the structure of comets; Atmospheric excitation of mars
polar motion; Dunite viscosity dependence on oxygen fugacity; Cross profile and volume analysis of bahram valles on mars;
Calculations of the fluxes of 10-250 kV lunar leakage gamma rays; Alluvian fans on mars; Investigating the sources of the
apollo 14 high-Al mare basalts; Relationship of coronae, regional plains and rift zones on venus; and Chemical differentiation
and internal structure of europa and callisto.
Derived from text
Atmospheric Circulation; Chemical Composition; Comets; Mars Surface; Lunar Rays; Gamma Rays; Basalt
20050170554 Jet Propulsion Lab., California Inst. of Tech., Pasadena, CA, USA
The Core of the Moon - Molten or Solid?
Khan, A.; Mosegaard, K.; Williams, J. G.; Lognonne, P.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In
English; See also 20050170551; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from
CASI on CD-ROM only as part of the entire parent document
While several studies beginning in the Apollo era and continuing up to the present have tried to detect the lunar core,
either geochemically, geophysically or geologically [e.g. 1, 2, 3, 4], it has so far proven somewhat elusive. The unambiguous

detection of the lunar core is of prime importance as it holds the potential of distinguishing between the various theories for
the formation of the Moon. The theory which currently enjoys the greatest success is the giant impact model, which has the
Moon forming about 4.5 Gyr ago from the debris produced when a Mars sized proto planet collided with the proto Earth [e.g.
5, 6]. Simulations reveal that the material from which the Moon is made up contains very little iron and consequently a lunar
core, if it exists, should be small.
Derived from text
Lunar Core; Moon; Iron
20050170555 Notre Dame Univ., IN, USA
Petrology of Nakhlite MIL 03346
Kinman, W. s.; Neal, C. R.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551;
Original contains color and black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on
CD-ROM only as part of the entire parent document
The new Nakhlite meteorite MIL- 03346 was found in Antarctica at the Miller Range of the Transantarctic Mountain
during the 2003-2004 field season. The exterior is approximately 60% covered by a black, wrinkled fusion crust. We were
allocated two samples from the 712.5g sample-a2gwhole rock sample and thin section MIL03346,9. Unfortunately, the
samples were received only 8 days before the abstract deadline so only a brief report comprised of mineralogical (electron
microprobe) data is reported here. The major and trace element data, including platinum-group element abundances, will be
reported at the conference.
Author
Nakhlites; Meteorites; Trace Elements
20050170556 Waseda Univ., Tokyo, Japan
Global Mapping of Elemental Abundance on Lunar Surface by SELENE Gamma-Ray Spectrometer
Kobayashi, M N.; Berezhnoy, A. A.; DUston, C.; Fujii, M.; Hasebe, N.; Hiroishi, T.; Kaneko, H.; Miyachi, T.; Mori, K.;
Maurice, S., et al.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original
contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the
entire parent document
Elemental composition on the surface of a planet is very important information for solving the origin and the evolution
of the planet and also very necessary for understanding the origin and the evolution of solar system. Planetary gamma-ray

spectroscopy is extremely powerful approach for the elemental composition measurement. Gamma-ray spectrometer (GRS)
will be on board SELENE, advanced lunar polar orbiter, and employ a large-volume Ge detector of 252cc as the main detector
[1]. SELENE GRS is, therefore, approximately twice more sensitivity than Lunar Prospector GRS, four times more sensitive
than APOLLO GRS. The high sensitivity of SELENE GRS will enable us to map element abundances of O, Mg, Fe, Al, Si,
Ti, K, Ca, Th, and U, with lower detection limit than the past missions. The Japanese lunar polar orbiter SELENE is scheduled
for launch in 2007 and the GRS will observe the whole area of the moon including the polar region. Orbiting the GRS at 100
km in a nominal operation for one year will provide the global mapping of the chemical composition of lunar surface material
for more elements than Lunar Prospector did [2]. Now, the flight model of SELENE GRS was built and will be qualified by
362
several environment test. Fig. 1 shows the schematic drawing. It shows an energy resolution of 3 keV @ 1.33 MeV in the GRS
system. In this study, we will exhibit expected performance of SELENE GRS in lunar orbits predicted by preliminary Monte
Carlo simulation results and describe scientific topics achievable by SELENE GRS.
Derived from text
Mapping; Gamma Ray Spectrometers; Lunar Maps; Lunar Surface; Planetary Surfaces; Abundance
20050170557 Oulu Univ., Finland
Mars Express HRSC Analysis of Two Impact Craters in Terra Tyrrhena, Mars
Korteniemi, J.; Kostama, V P.; Aittola, M.; Ohman, T.; Tormanen, T.; Lahtela, H.; Raitala, J.; Neukum, G.; Lunar and
Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original contains color illustrations;
Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
The surface of Mars is governed by division to smooth northern lowlands and intensely cratered highland terrain in the
south. The cratering record indicates the age of the surface [e.g. 1,2], while individual craters original morphology hints to
the target material at the time of impact [3]. Additionally, the craters provide natural sinks for later deposited materials, thus
showing glimpses of the evolution of the region they reside in. In all, craters provide information on the local and areal
evolution phases and processes.
Derived from text
Cratering; Mars Craters; Morphology; Mars Surface; Terrain
20050170558 Academy of Sciences (USSR), Moscow, USSR
The Martian North Polar Cap Spirals are the Traces of an Ancient Ice Sheet Collapse
Kostrikov, A. A.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original

contains color and black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM
only as part of the entire parent document
The surface of north polar cap of Mars is essentially heterogeneous unlike flat terrestrial ice sheets [1]. Troughs up to one
kilometer deep with gently (no more 10-15 ) sloping are seen all over the ice cap. The unique feature of the trough system
is its helical appearance (Fig. 1). Analogs of ice spiral structures are not known. The troughs have been attributed to the action
of aeolian erosion [2-3], sublimation [4] or to ‘accublation’ hypothesis (glacial flow + sublimation + accumulation) [5-7]. It
is supposed that an ice mass transfer occurs by sublimation from equatorward-facing slopes and subsequent accumulation on
pole-facing slopes. No ideas on origin of spiral pattern have been moved forward with the exception of an attempt to explain
trough revolving by combined effects of accublation and ice movement [8].
Derived from text
Collapse; Ice; Glaciers; Polar Caps; Mars Surface
20050170560 Russian Academy of Natural Sciences, Moscow, Russia
Wind-related Erosion Depressions Within a Small Impact Craters in Chryse and Elysium Planitiae on Mars
Kuznetsov, I. V.; Kuzmin, R. O.; Greeley, R.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See
also 20050170551; Original contains color and black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy;
Available from CASI on CD-ROM only as part of the entire parent document
High resolution Mars Orbiter Camera (MOC) images [1] show wide variety of the aeolian features within the impact
craters attributed to wind erosion and deposition: different types of bright and dark crater streaks, duneforms, bright transverse
dunes, interacrater deposits, and rim scouring forms. The orientation of these aeolian features is consistent with the direction
of current strong winds [2,3], while origin of some of them could be related with paleowind regime[4]. Here we present the
results of study of unknown before phenomenon of the wind-related modification of the impact craters on Mars in the form
of blowout hollows which have been found only in two places on Mars: much more in southern part of Chryse Planitia (CP)
and less in south-western part of Elysium Planitia (EP).
Derived from text
Dunes; Mars Craters; Wind Erosion; Wind (Meteorology); Mars Surface
20050170561 Belgian Royal Observatory, Brussels, Belgium
Atmospheric Excitation of Mars Polar Motion
Karatekin, O.; Dehant, V.; deViron, O.; VanHoolst, T.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 1 pp.; In

English; See also 20050170551; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of
the entire parent document
363
The rotation of Mars is not constant and present irregularities with time. Those are mostly associated with the seasonal
cycle of Mars’ atmosphere, and the condensation/sublimation of the icecaps. The dynamics of Mars atmosphere shows a large
annual and semi-annual signal, in addition to the diurnal cycle. Besides those periodic components, in the present study we
investigate the other atmospheric effects that can excite the polar motion. The influence of surface/atmosphere interactions on
the rotation dynamics is classically estimated using the angular momentum approach. The Mars-atmosphere system is
considered as isolated, so that any change in the atmosphere angular momentum is associated with an opposite change in the
planetary angular momentum. The angular momentum of the atmosphere can be separated into two parts: a matter term
representing the rigid rotation of the fluid layer with the planet, and a wind term accounting for the relative motion of the fluid
with respect to the surface of the planet.
Derived from text
Rotation; Mars Atmosphere; Planetary Surfaces; Atmospheric Circulation; Excitation; Surface Reactions
20050170563 Academy of Sciences (Russia), Moscow, Russia
The Smerdyacheye Lake: New Evidence for Impact Origin and Formation Age
Kashkarov, L. L.; Badijukov, D. D.; Ivliev, A. I.; Kalinina, G. V.; Nazarov, M. A.; Lunar and Planetary Science XXXVI, Part
11; [2005]; 2 pp.; In English; See also 20050170551; Original contains color illustrations; Copyright; Avail: CASI;
A01,
Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
The Smerdyacheye Lake of about 350 m in diameter is located in the Moscow district approximately 140 km east of
Moscow. This lake has a circular shape and a well-developed rim. Based on the features, it has been suggested that the lake
is a possible meteorite crater. The suggestion was confirmed by a fragment of a possible impactite found in the rim. In this
paper we report on a glass bead discovered recently in the vicinity of the lake. In composition and texture the glass is similar
to impact-glasses and supports strongly impact origin of the lake. First data on fision track age and TL characteristics of this
glass bead are reported.
Author
Meteorite Craters; Age Factor; Beads; Glass; Lakes
20050170564 Idaho Univ., Moscow, ID, USA

Compressive Anti-Cracks at the Tips of Strike-Slip Faults on Europa and Implications for Fault Mechanics
Kattenhorn, Simon A.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551;
Original contains black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM
only as part of the entire parent document
Secondary fractures, or tail-cracks, at the tips of strike-slip faults are common on Europa and form in response to
high-magnitude tensile stresses induced by fault slip. However, linear elastic fracture mechanics theory (LEFM) predicts both
extensional and compressive quadrants around fault tips. Theoretically, these quadrants can be associated with tensile
secondary fracturing (cracks) and compressive secondary fracturing (anti-cracks), respectively. The existence of such features
in terrestrial rocks has been widely documented.
Derived from text
Fracture Mechanics; Geological Faults; Europa; Cracks
20050170567 University of Western Ontario, London, Ontario, Canada
Comparison of Predicted Salt Precipitation Sequences with Mars Exploration Rover Data
King, P. L.; Lescinsky, D. T.; Nesbitt, H. W.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See
also 20050170551; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire
parent document
We compare predicted salt sequences for Mars with Mars Exploration Rover (MER) data to place constraints on martian
waters. On Mars, geomorphic and geochronologic evidence suggest that surface solutions occurred episodically, and chemical
evidence suggests limited weathering of the basaltic crust. Saline solutions are produced via leaching of bulk martian surface
materials (martian and impactor materials) containing sulfides, olivine, pyroxene, plagioclase glass. The resulting bulk
solution would contain Mg-Ca-Na-(K-Fe)-C-O-H-S-(N-P)- halogen species, with abundant Mg, Na, SO4 and Cl. Local
compositional variations are likely. On Mars, sulfate stays in solution, unlike on Earth where sulfate is reduced to sulfide either
via biologic processes or hydrothermally at mid-ocean ridges. We model the martian solution compositions as they are
concentrated (via freezing or evaporation) using salt solubility and phase equilibria, assuming: 1) thermodynamic modeling
364
is appropriate; 2) 25 C and approx. 10(exp 5) Pa phase diagrams are valid at martian conditions; and, 3) activity coefficients
are unity.
Derived from text

Sodium Chlorides; Precipitation (Chemistry); Mars Exploration; Mars Surface; Data Processing
20050170569 Wisconsin Univ., Madison, WI, USA
Correlation Between Aluminum-26 Ages and Bulk Si/Mg Ratios for Chondrules from LL3.0 - 3.1 Chondrites
Kita, N. T.; Tomomura, S.; Tachibana, S.; Nagahara, H.; Mostefaoui, S.; Morishita, Y.; Lunar and Planetary Science XXXVI,
Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original contains color illustrations; Copyright; Avail: CASI;
A01,
Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
Recently, the Al-26 - Mg-26 analyses were performed for many chondrules from least equilibrated chondrites by using
ion microprobe. The initial Al-26/Al-27 ratios of these chondrules are between 1.5 x 10(exp -5) and 3 x 10(exp -6), 1-3 million
years (Myr) younger than CAIs with the canonical initial ratios of 5 x 10(exp -5). Similar age differences between CAIs and
chondrules are also reported from absolute Pb-Pb ages. Thus, the initial Al-26/Al-27 ratio of the solar system is considered
to be homogeneous for applying the Al-26 - Mg-26 chronometer.
Derived from text
Aluminum Isotopes; Age Factor; Silicon; Chondrule; Chondrites; Meteoritic Composition; Magnesium Isotopes
20050170570 Muenster Univ., Germany
The Hf-W Age of the Lunar Magma Ocean
Kleine, T.; Mezger, K.; Palme, H.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also
20050170551; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent
document
The early chemical differentiation of the Moon was dominated by the crystallization of a magma ocean. Determining the
crystallization age of the lunar magma ocean (LMO) is critical for understanding the timing of Moon formation, melting, and
subsequent differentiation and cooling. Currently, the most suitable isotope system for dating the crystallization of the LMO
is the Hf-182 - W-182 decay scheme, because the Hf/W ratios varied significantly between the different LMO reservoirs, and
W isotope variations can have only been produced in the first approx. 60 Myr of the solar system. Thus, information on early
differentiation of the Moon is preserved in the 182W/184W of early-formed lunar reservoirs and is carried by lunar samples
derived from any of these sources. A chronological interpretation of W isotope ratios for lunar whole-rocks and minerals,
however, has been hampered by the neutron-flux induced production of W-182 from Ta-181 caused by the intense cosmic
radiation reaching the surface of the Moon. Analyzing the metals of lunar samples can overcome this problem because metals
do not contain significant Ta that could be converted to W-182. We present W isotope data for metals from KREEP-rich and

-poor highland breccias and low-Ti and high-Ti mare basalts. To investigate the effect of cosmogenic W-182 production in
whole-rock samples, the W isotopes in some whole-rocks have also been analyzed
Author
Hafnium Isotopes; Tungsten Isotopes; Age Factor; Lunar Geology; Magma; Oceans; Crystallization
20050170571 Muenster Univ., Germany
Tungsten Isotopes Provide Evidence that Core Formation in Some Asteroids Predates the Accretion of Chondrite
Parent Bodies
Kleine, T.; Mezger, K.; Scherer, E.; Palme, H.; Scherer, E.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In
English; See also 20050170551; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of
the entire parent document
Chondrites are generally assumed to be the most primitive rocks of the solar system and to represent the precursor
material from which asteroids accreted and then differentiated. Chondrites contain CAIs and chondrules, the former
representing the oldest yet dated material formed in the solar system. Age differences between CAIs and chondrules based on
the U-Pb and 26Al-26Mg chronometers show that chondrule formation persisted for at least approx. 2.5 Myr, indicating that
accretion of chondrite parent asteroids lasted for at least approx. 2.5 Myr. These results contrast with estimates from planetary
accretion models that propose that the first planetary objects formed within 1 Myr after condensation of the first solid matter.
Hf-182 - W-182 ages for iron meteorites show that differentiation (i.e., core formation) of their parent bodies occurred within
approx. 5 Myr of each other. For the first time, we link this differentiation event to the ages of CAIs, chondrules, and chondrite
365
parent asteroids, by applying the Hf-182 - W-182 chronometer to CAIs, primitive chondrites, and iron meteorites.
Author
Tungsten Isotopes; Planetary Cores; Asteroids; Chondrites; Meteoritic Composition; Hafnium Isotopes
20050170573 Aizu Univ., Fukuyama, Japan
Shape Modeling for the Asteroid (25143) Itokawa, AMICA of Hayabusa Mission
Kobayashi, S.; Demura, H.; Asada, N.; Furuya, M.; Hashimoto, T.; Saito, J.; Lunar and Planetary Science XXXVI, Part 11;
[2005]; 1 pp.; In English; See also 20050170551; Original contains color and black and white illustrations; Copyright; Avail:
CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
Hayabusa established Earth-swingby a success in May 12, 2004 and the spacecraft is on course to the target asteroid

Itokawa. Hayabusa mission is a sample return program of ISAS/JAXA. The spacecraft is going to arrive at Itokawa and to
touch down on the surface for sampling materials in autumn of 2005. Our science team requires 3D shape model of the
asteroid, which provides fundamental information for making a decision on selecting landing sites. Nowadays, image-based
modeling is the favored method of shape recognition of asteroids. For example, Wild 2 was recognized its irregular shape by
stereo images. We found following problems make it difficult to develop the precise shape model by stereo method; (1)
Hayabusa is equipped a single-eyed camera, (2) Hayabusa doesn’t know own exact position enough to ordinary stereo method.
Here we report the procedures and results of this modeling with AMICA (Asteroid Multiband Imaging Camera) and attitude
of spacecraft, and distance between target asteroid and the spacecraft only.
Derived from text
Three Dimensional Models; Sample Return Missions; Imaging Techniques; Cameras; Asteroid Missions; Shape Optimization
20050170574 Wien Univ., Austria
The 2004 ICDP Bosumtwi Impact Crater, Ghana, West Africa, Drilling Project: A First Report
Koeberl, Christian; Milkereit, B.; Overpeck, J. T.; Scholtz, C. A.; Peck, J.; King, J.; Lunar and Planetary Science XXXVI, Part
11; [2005]; 2 pp.; In English; See also 20050170551; Original contains color illustrations
Contract(s)/Grant(s): NSF-ATM-04-02010; ANSF Proj. P17120-N10; Copyright; Avail: CASI;
A01, Hardcopy; Available
from CASI on CD-ROM only as part of the entire parent document
The 10.5-km-diameter 1.07 Ma Bosumtwi impact crater was the subject of an interdisciplinary and international drilling
effort of the International Continental Scientific Drilling Program (ICDP) from July to October 2004. Sixteen different cores
were drilled at six locations within the lake, to a maximum depth of 540 m. A total of about 2.2 km of core material was
obtained.
Author
Geophysics; Ghana; Lunar Craters; Seismology; Drilling
20050170575 International Research School of Planetary Sciences, Pescara, Italy
Morphology and Morphometry of Fluidized Ejecta Blankets: New Results from the Mars Express High Resolution
Stereo Camera
Komatsu, G.; Ori, G. G.; DiLorenzo, S.; Rossi, A. P.; Neukum, G.; Lunar and Planetary Science XXXVI, Part 11; [2005];
2 pp.; In English; See also 20050170551; Original contains color and black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
Impact craters on Mars often exhibit features that are not observed on the Moon. The most unusual is the ejecta blanket

morphology. Martian ejecta blankets are in general characterized by a terminal low concentric ridge (rampart) or a flat-topped
plateau (pancake), or radial grooves and scouring. This type of ejecta morphology collectively called layered ejecta structures
is in general attributed to various ejecta displacement processes due to involvement of volatiles derived from the subsurface
or of atmosphere. We utilized images and stereo-derived topographic data acquired by the HRSC (High Resolution Stereo
Camera) onboard Mars Express in order to study geology of Martian impact crater ejecta blankets. We examined more than
a dozen impact craters with possible evidence for water involvement during the formation by constructing 3-dimensional
views and deriving various parameters. The high precisions of the HRSC data set ensure quantitative analyses of such impact
craters better than previously possible. The investigated relatively pristine impact craters are distributed in the eastern Tharsis,
but examples from other regions are also included. We examined various geomorphology and geomorphic parameters of
Martian layered ejecta structures. The layered ejecta structures on Mars have been classified into different types including
single lobe, multi lobate and double lobate. Representative topographic profiles from our study clearly show a wide range of
morphology. An example of typical single-lobed layered ejecta structure is shown having a thick flat-topped plateau and a
366
terminal rampart. The double lobate type is characterized by clearly separate inner thick lobes and much thinner outer lobes.
Derived from text
Cameras; Ejecta; Geomorphology; High Resolution; Mars Express; Stereophotography; Mars Craters
20050170577 Arizona State Univ., Tempe, AZ, USA
Palagonite-like Alteration Products on the Earth and Mars 2: Secondary Mineralogy of Crystalline Basalts Weathered
Under Semi-Arid Conditions
Kraft, M. D.; Michalski, J. R.; Sharp, T. G.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also
20050170551; Original contains black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI
on CD-ROM only as part of the entire parent document
The Martian surface may be mineralogically altered from its pristine, igneous state. Aqueous alteration on Mars would
lead to formation of secondary minerals, which could occur in soils, weathering rinds, rock coatings, or sedimentary cements.
In order to understand the alteration state of the Martian surface, it is crucial that we anticipate what secondary minerals might
have formed on Mars. It is also critical that we understand how secondary materials affect remote observations. In particular,
we must understand spectral observations of secondary minerals in geologic context: How do these materials appear when they
occur as weathering rinds, soils, cements, or coatings? Small amounts of weathering could produce significant differences
between fresh rock and weathered rock spectra. Previously, we investigated thermal infrared spectra of silica-coated rocks and

showed that small amounts of amorphous silica coating basalt greatly influenced spectra, with silica coatings thicker than 7-10
m completely obscuring the basalt s thermal infrared spectral signature [1]. In weathering rinds, fine-grained, secondary
silicates tend to coat primary minerals, and can be thought of as discontinuous, rock-penetrating coatings. Consequently, we
expect thermal infrared spectral effects of weathering rinds to be similar to those seen with silica coatings, in that small
volumes of secondary products will have large effects.
Derived from text
Planetary Geology; Mineralogy; Crystallinity; Basalt; Temperature Effects; Silicon Dioxide
20050170579 Moscow State Univ., Russia
The Gagarin Ring Structure, Russia: A Possible Meteorite Crater
Krivosheya, K. V.; Badyukov, G. D.; Badjukov, D. D.; Raitala, J.; Lunar and Planetary Science XXXVI, Part 11; [2005];
2 pp.; In English; See also 20050170551; Original contains color and black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
The Gagarin ring structure has been described as a proposed meteorite crater in 1975. The assumption was based on
morphological details of the structure and geophysical data. Here we report new data which support the possible impact origin
of the structure.
Derived from text
Geophysics; Meteorite Craters; Structural Properties (Geology); Mineralogy; Russian Federation
20050170580 Academy of Sciences (USSR), Moscow, USSR
Chemical Differentiation and Internal Structure of Europa and Callisto
Kuskov, O. L.; Kronrod, V. A.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also
20050170551; Original contains color illustrations
Contract(s)/Grant(s): RFBR-03-05-64413; RFBR-04-05-64867; Copyright; Avail: CASI;
A01, Hardcopy; Available from
CASI on CD-ROM only as part of the entire parent document
The purpose of this study is to reproduce characteristic features of the internal structure of Europa and Callisto on the basis
of Galileo gravity measurements, geochemical constraints on composition of silicate fraction of ordinary and carbonaceous
chondrites, and thermodynamic data on the equations of state of water, high-pressure ices, and meteoritic material.
Derived from text
Chemical Composition; Europa; Callisto; Galileo Spacecraft; Geochemistry; Gravitation; Meteoritic Composition
20050170581 Kharkiv State Univ., Kharkiv, Ukraine

Studying the Phase Dependence of Lunar Surface Brightness Using Data of Integral Observations
Korokhin, V. V.; Velikodsky, Yu, I.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also
20050170551; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on
CD-ROM only as part of the entire parent document
367
Lane and Irvine carried out the integral photometrical observations of the Moon at Le Houga observatory (South France)
in 1964-1965. These are the most full integral observations of the Moon: the Moon was observed over phase angles 6 degrees
less than or equal to alpha less than or equal to 120 degrees in nine narrow bands (350-1000 nm) and in UBV. But their
suitability for studying the phase dependence of brightness of lunar surface decreases through presence of systematical errors
caused by influence of libration variations and changing of contribution of mares and highlands in integral brightness with
phase changes. Therefore we have tried to correct Lane’s and Irvine’s data.
Derived from text
Brightness; Lunar Surface; Photometry; Moon; Data Processing
20050170584 California Univ., Los Angeles, CA, USA
Siderophile Geochemistry of Ureilites: Reading the Record of Early Stages of Planetesimal Core Formation
Kallemeyn, Gregory W.; Warren, Paul H.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also
20050170551; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on
CD-ROM only as part of the entire parent document
Ureilites, the second most abundant type of achondrite, formed as partial melt restites (olivine + pyroxene + minor, 0.2-6
wt%, carbon) in the mantles of carbonaceous asteroids. Degrees of melting were sufficient to virtually eliminate plagioclase
from the entire ureilite milieu; at temperatures of approx.1210- 1300 C [1]. According to some recent interpretations [e.g., 2,3]
core formation commences not long after an asteroidal interior reaches the Fe-FeS eutectic (approx.990 C). This scenario
seems implausible for the interior of an asteroid, where extensive mobilization of solid components (without implausibly high
S, only minor proportions of metal will melt near the eutectic) can only be expected as a concomitant of extensive matrix
melting. At any rate, at about the same time the ureilites underwent partial melting, they acquired moderate to major depletions
in siderophile elements. Natural siderophile variations are notoriously untidy, but collectively the many ureilite samples can
potentially furnish important insight into the early stages of core formation.
Derived from text

Ureilites; Protoplanets; Olivine; Geochemistry; Melting; Carbon
20050170585 Oklahoma Univ., Norman, OK, USA
Large Eddy Simulation of Coherent Structures and Dust Devil-like Vortices in the Martian Boundary Layer
Kanak, K. M.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original
contains color and black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM
only as part of the entire parent document
Dust devils are columnar convective vortices made visible by the presence of dust or other particulates. They occur most
often in environments characterized by low ambient wind speeds and strong unstable lapse rates. There is increasing evidence
that vertical vortices in the terrestrial convective boundary layer may occur frequently without the presence of visible tracers
and therefore be much more common than previously thought. The ubiquity of dust devil tracks in certain regions on Mars
suggest that they are a regular feature of the Martian boundary layer. The implications of dust devils on vertical transports of
heat, momentum, and particulates may be significant. In addition, they could pose some threat to landers and rovers, or
spacecraft upon descent and landing. This study presents results from an idealized Large Eddy Simulation (LES) of the
Martian Boundary Layer (MBL). Comparisons are made with prior Martian dust devil modeling study results, in which
different numerical models were used and with observations.
Author
Coherence; Dust; Vortices; Mars Surface; Boundary Layers; Large Eddy Simulation
20050170586 Brown Univ., Providence, RI, USA
Analysis of Martian Pyroxene Compositions in Syrtis Major: Full MGM Application to OMEGA
Kanner, L. C.; Mustard, J. F.; Bibring, J-P.; Gendrin, A.; Langevin, Y.; Gondet, B.; Pelkey, S.; Lunar and Planetary Science
XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original contains color illustrations; Copyright; Avail:
CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
Spectra from the OMEGA visible-infrared spectrometer [1] of the Syrtis Major region of Mars are analyzed for pyroxene
composition and the relationships to local geologic units. Individual spectra were analyzed using the Modified Gaussian Model
(MGM) [2]. Final MGM fits indicate the presence of two pyroxenes in Syrtis Major, in agreement with previous studies [3,
368
4]. The results indicate that the old cratered terrains are low-calcium pyroxene rich while the overlying volcanic province is
high-calcium pyroxene rich. Olivine is likely present in some regions.

Author
Pyroxenes; Mars Surface; Infrared Spectrometers; Craters
20050170587 Geological Survey, Flagstaff, AZ, USA
Aqueous Chemistry, Physical Chemistry, and Sedimentology of Rocks at the Mars Rover Landing Sites
Kargel, J. S.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original
contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the
entire parent document
The Mars Exploration Rovers, Opportunity and Spirit, have provided critical ground truth observations pertinent to global
data sets and observations that have been interpreted in terms of an aqueous past. Most crucial from these new rover missions
has been their ability to travel to rock outcroppings and probe the weathered exteriors and fresher interiors of rocks with
chemical and mineralogical and a variety of optical imaging systems. Both rovers have returned data indicating layer-by-layer
aqueous deposition or aqueous alteration under conditions that were almost certainly highly acidic and hypersaline but not as
cold as current conditions. The two landing sites are very different, but the rover observations dovetail nicely with synoptic
observations made from orbiters. The accumulated sets of observations for both sites indicate periods of hydrogeologic
processes involving huge amounts of liquid water. Both rovers have produced data consistent with possible continued aqueous
processes, most likely involving minute traces of acidic, saline brines that are liquid and chemically active in the upper
centimeters on warm days, but frozen much of the time. Terrestrial analog sites provide a rich variety of insights into the cause
of the observed chemistry, mineralogy, and physical sedimentology at each rover site. A sea or big lake is implicated for
Meridiani Planum, and a huge debris flow is likely at Gusev Crater. Room remains for alternate or modified interpretations,
but water is unavoidable.
Author
Mars Surface; Mineralogy; Physical Chemistry; Sedimentary Rocks
20050170588 Museum of Natural History, London, UK
Interpreting Micrometeoroid Residues on Metallic Spacecraft Surfaces: Clues from Low Earth Orbit, the Laboratory
and to Come from Stardust?
Kearsley, A. T.; Burchell, M. J.; Graham, G. A.; Cole, M. J.; Wallis, D.; Lunar and Planetary Science XXXVI, Part 11; [2005];
2 pp.; In English; See also 20050170551; Original contains color and black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
Surfaces of spacecraft returned from low Earth orbit (LEO) preserve a record of high velocity collisions with small (less

than 1mm) particles. Surveys of features on metal, glass and other materials have identified remains of micrometeoroids.
Analytical electron microscopy using energy dispersive X-ray spectrometry (EDS) has proven very successful in distinction
of impacts by artificial and natural particles, and holds promise for interpretation of micrometeoroid residues in terms of
particle origin.
Derived from text
Micrometeoroids; Residues; Metallic Glasses; Surface Layers; Spacecraft Shielding
20050170589 NASA Johnson Space Center, Houston, TX, USA
In-Situ Heating Decrease Kinetics of Aliphatic Hydrocarbons in Tagish Lake Meteorite by Micro-FTIR
Kebukawa, Y.; Nakashima, S.; Zolensky, M. E.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See
also 20050170551; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on
CD-ROM only as part of the entire parent document
Carbonaceous chondrites are known to contain up to 3wt.% C, the major part of which corresponds to a macromolecular
organic fraction. Chondritic organic matter is based on small aromatic units, cross-linked by short aliphatic chains rather than
large clusters of polyaromatic structures. Two main characteristic features of those organics measured by FTIR are: (1) an
equivalent intensity of the asymmetric stretching mode absorptions for CH3 (2960/cm) and CH2 (2920/cm) and (2) a lack of
aromatic CH-stretching mode (3040/cm). Tagish Lake is a new type of water- and carbon-rich type 2 carbonaceous chondrite.
Its total carbon content is approx. 5 wt%, of which the organic carbon content reaches approx. 1.3 wt%. Tagish Lake may have
never experienced temperatures higher than 120 C after formation of organics based on the disappearance of infrared (IR)
organic peaks in step heating experiments. Here we report in-situ kinetic heating experiments of organics in Tagish Lake by
369
micro-FTIR to characterize the nature of aliphatic hydrocarbons and their thermal stabilities.
Author
In Situ Measurement; Kinetic Heating; Aliphatic Hydrocarbons; Lakes; Meteorites
20050170590 Minnesota Univ., Minneapolis, MN, USA
Dunite Viscosity Dependence on Oxygen Fugacity
Keefner, J. W.; Mackwell, S. J.; Kohlstedt, D. L.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English;
See also 20050170551; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire
parent document

A detailed understanding of the behavior of dunite flow is crucial because small errors in a laboratory-derived constitutive
equation become large errors when extrapolated to mantle conditions. The oxidation state of the upper mantle of the Earth,
Mars, and Venus may play a role in the development of endogenic processes that lead to observable surface features. Oxygen
fugacity is known to have an effect on the viscosity of olivine single crystals under constant stress. However, the behavior of
polycrystalline olivine samples deformed under different oxidation states is less well understood. Deformation experiments
were performed on Aheim dunite over ranges of temperature, stress, and solid state buffer to investigate the dependence of
viscosity on oxygen fugacity. In many studies of kinetic properties on olivine single crystals and polycrystalline aggregates,
oxygen fugacity was buffered at the iron-wustite (IW) buffer by the sample jacket. In the present study, we explicitly compare
the strength of samples deformed at the nickel-nickel oxide (NNO) and the iron-wustite solid state buffers in order to quantify
the dependence of creep rate on oxygen fugacity.
Author
Dunite; Viscosity; Oxygen; Planetary Mantles
20050170592 NASA Goddard Space Flight Center, Greenbelt, MD, USA
Pickup Ion Mass Spectrometry for Surface Bounded Exospheres and Composition Mapping of Lunar and Planetary
Surfaces
Keller, J. W.; Zurbuchen, T. H.; Baragiola, R. A.; Cassidy, T. A.; Chornay, D. J.; Collier, M. R.; Hartle, R. E.; Johnson, R. E.;
Killen, R. M.; Koehn, P., et al.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also
20050170551; Original contains color and black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available
from CASI on CD-ROM only as part of the entire parent document
Many of the small to medium sized objects in the solar system can be characterized as having surface bounded
exospheres, or atmospheres so tenuous that scale lengths for inter-particle collisions are much larger than the dimensions of
the objects. The atmospheres of these objects are the product of their surfaces, both the surface composition and the
interactions that occur on them and also their interiors when gases escape from there. Thus by studying surface bounded
exospheres it is possible to develop insight into the composition and processes that are taking place on the surface and interiors
of these objects. The Moon and Mercury are two examples of planetary bodies with surface bounded exospheres that have
been studied through spectroscopic observations of sodium, potassium, and, on the moon, mass spectrometric measurements
of lunar gases such as argon and helium.
Derived from text
Planetary Surfaces; Lunar Surface; Mass Spectroscopy; Ions; Exosphere; Mapping; Surface Layers; Gas Analysis

20050170594 University of Southern Georgia, Statesboro, GA, USA
Analysis of the Statesboro, Georgia Shock-darkened L5 Chondrite
Kelley, Michael S.; Asher, Pranoti M.; Welten, Kees C.; Jull, A. J. TImothy; Schultz, Ludolf; Roden, Michael; Mertzman,
Stanley A.; Albin, Ed F.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551;
Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
In August 2003, Statesboro, Georgia farmer Harold Cannon brought an unusual rock to the Department of Geology and
Geography at Georgia Southern University. There are few naturally occurring rocks on the coastal plain of Georgia, so by
definition, any rock found there is ‘unusual’. However, this particular specimen turned out to be not only unusual, but
otherworldly. In mid-June, 2000 Cannon was harvesting a crop of butter beans when his mechanical bean picker pulled the
rock up from his field. In the process, yellow paint from the device was deposited on the specimen. Cannon removed the rock
and tossed it between a pair of produce freezers under a shed in his back yard. For more than 3 years the rock sat exposed
to the elements. When Cannon was cleaning the area around the shed in summer 2003, he finally decided to find out exactly
370
what the rock was. He said he suspected it might be a meteorite because it was heavier than expected for its size, and after
breaking off a small fragment, he noticed it was very dark inside.
Derived from text
Chondrites; Meteorites
20050170595 Museum fuer Naturkunde, Berlin, Germany
Thin-Skin Delamination of Target Rocks Around the Ries Crater: The Effect of Spallation and Ejecta Drag
Kenkmann, T.; Ivanov, B. A.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551;
Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part
of the entire parent document
The Ries crater is the best suited large impact crater on Earth to study processes of excavation and near-surface
deformation of target rocks as the amount of erosion is minor. We have analysed the deformation of parautochthonous and
autochthonous target rocks inside and outside the tectonic crater rim at a distance ranging from 10 to 20 km with respect to
the crater center. We have observed several sub-horizontal shear planes (detachments) in stratified target rocks and measured
their displacement vector. It is suggested that spallation and dragging of the ejecta curtain caused the formation of detachments
in the surrounding of the transient crater cavity. Anumerical model is compared with the structural data and gives further hints

to the time sequence, applied stresses, and magnitude of shear movements.
Derived from text
Craters; Deformation; Displacement; Tectonics; Delaminating
20050170596 Jet Propulsion Lab., California Inst. of Tech., Pasadena, CA, USA
Dual Balloon Concept for Lifting Payloads from the Surface of Venus
Kerzhanovich, Viktor V.; Yavrouian, A. H.; Hall, J. L.; Cutts, J. A.; Lunar and Planetary Science XXXVI, Part 11; [2005];
2 pp.; In English; See also 20050170551; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy;
Available from CASI on CD-ROM only as part of the entire parent document
Introduction: Two high-rated Venus mission concepts proposed in the National Science Foundation Decadal Survey
require a balloon to lift payloads from Venusian surface to high altitudes: Venus Surface Sample Return (VESSR) and Venus
In-Situ Explorer (VISE). In case of VESSR the payload is a canister with the surface sample plus a Venus ascent vehicle
(VAV), which is a rocket that takes the sample into orbit for rendezvous with an Earth return vehicle. VISE is envisioned as
a more limited precursor mission where the surface sample is only taken to high altitudes so that non time-critical analyses
can be performed. From the balloon point of view, the only difference between these two missions is that the VESSR payload
to be lifted is very much larger than VISE because of the inclusion of the VAV. A key problem is that at the time the decadal
survey was published, no high temperature balloon technology existed to implement either mission. Prior technology
development efforts had concentrated on a single balloon that could operate across the entire 0-60 km altitude range, tolerating
both the sulfuric acid aerosols and the extreme temperatures of -10 to +460 C. However, this problem was unsolved because
no combination of sufficiently lightweight balloon material and manufacturing (seaming) technology was ever found to
tolerate the high temperatures at the surface.
Author
Balloons; Venus Surface; Orbital Rendezvous; Sample Return Missions; Payloads
20050170598 Geological Survey, Flagstaff, AZ, USA
Some Simple Models for Rootless Cone Formation on Mars
Keszthelyi, L.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original
contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the
entire parent document
Volcanism provides a unique tool to sound for water in Mars geologic past. The interaction between molten lava and

surface and ground water produces a range of morphologic features on Earth. Many of these features are interpreted to exist
on Mars. Rootless cones (a.k.a. pseudocraters) have been reported in a number of locations on Mars and interpreted to be the
result of explosive interaction between the liquid lava and groundwater/ice. The enigmatic ring structures seen in Athabasca
Valles may have formed by relatively gentle lava-groundwater interaction. Mesas-like features in several areas of Mars are
interpreted as constructional features formed by lava erupted under ice and/or water. However, rootless cones remain the
feature most often and definitively cited as evidence of lava-water interaction on Mars. Despite the repeated use of these
rootless cones to infer the presence of water in the shallow subsurface, only limited quantitative information has been extracted
371
from them. The minimum depth to subsurface water or ice has been calculated based on the simple assumption that the lava
must conductively heat the substrate, melt ice, and boil water. Greeley and Fagents also calculate the amount of gas needed
to propel clasts to build a rootless cone on Earth and Mars. They concluded that only small amounts of water are necessary
for rootless cones to form on Mars. Simple Steam Accumulation Model: In rootless
Author
Ground Water; Lava; Mars Craters; Planetary Geology; Ring Structures
20050170599 Geological Survey, Flagstaff, AZ, USA
Reconciling Lava Temperatures and Interior Models for Io
Keszthelyi, L.; Milazzo, M.; Jaeger, W. L.; Wilson, L.; Mitchell, K. L.; Lunar and Planetary Science XXXVI, Part 11; [2005];
2 pp.; In English; See also 20050170551; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy;
Available from CASI on CD-ROM only as part of the entire parent document
The very high temperatures that have been reported for lavas on Io have proven to be difficult to explain. In particular,
the estimates of lava temperatures of approx. 1600 C require that the interior of Io be: (a) largely undifferentiated and (b)
almost completely molten. However, models of tidal dissipation within Io show that a largely molten interior would not
produce sufficient heat to maintain the observed level of volcanism. The latest modeling suggests that Io s mantle should not
contain more than 20% melt. If Io s bulk composition is similar to a CM chondrite, then 20% melt implies a lava temperature
of 1200 C. This 400 C discrepancy is the focus of this study.
Derived from text
Lava; High Temperature; Io
20050170601 Lunar and Planetary Inst., Houston, TX, USA
Gravity Models of the Hemispheric Dichotomy in Eastern Mars: Lithospheric Thickness and Subsurface Structure

Kiefer, Walter S.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original
contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the
entire parent document
The hemispheric dichotomy of Mars is one of the most prominent topographic structures on the planet, with a typical
offset of 4 km between the southern highlands and the northern lowlands. Various mechanisms have been proposed for forming
the dichotomy, including both internal processes related to mantle convection and external processes related to one or more
large impacts. Gravity and topography observations provide clues that can help to constrain the mechanisms which produced
the dichotomy. For example, these observations can constrain the lithospheric thickness and hence the heat flux at the time
of lithospheric loading. They can also reveal the presence of possible buried structures. In this work, I focus on the dichotomy
boundary in eastern Mars between 50o and 155o East longitude. In this region, the dichotomy boundary has a roughly linear
planform, striking NW-SE, except where the boundary is affected by the Isidis impact basin. The topographic offset across the
dichotomy in this part of Mars is relatively scarp-like, with 3 to 4 km of vertical relief occurring across a narrow transition
zone between the southern highlands and the northern lowlands. The results reported here are based on the highest resolution
gravity model currently available from the Planetary Data System, JGM95I-01, and include spherical harmonic degrees 2-60
(half-wavelength resolution 180 km).
Author
Gravitation; Dichotomies; Mathematical Models; Mars Surface; Lithosphere; Structural Basins; Thickness
20050170602 New Mexico Univ., Albuquerque, NM, USA
Calculations of the Fluxes of 10-250 keV Lunar Leakage Gamma Rays
Kim, K. J.; Reedy, R. c.; Gasnault, O.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also
20050170551; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on
CD-ROM only as part of the entire parent document
The gamma rays measured above the surface of planetary objects can be used to study that surface s composition.
Previous and current measurements have mainly used gamma rays with energies greater than 500 keV, although most missions
measured down to approx. 100 keV. Gamma rays above approx. 100 keV are very penetrating and thus hard to collimate, so
previous missions to the Moon and Mars have measured gamma rays arriving from the entire visible surface. The spatial
resolution was not better than about the distance above the planet s surface. The continua observed on previous missions down
to ~100 keV increases significantly with decreasing energy. These continua make it hard to measure the fluxes of gamma-ray

lines with energies below approx. 500 keV, and all elemental analyses have used higher-energy gamma rays, usually using only
372
lines. The continuum can be used to study components of the lunar composition. The lunar continuum is a good measure of
the abundance of the natural radioactive elements K, U, and Th, using the continuum between 0.55 and 2.75 MeV and between
450 and 480 keV. Fourier transforms of continua have been proposed to determine composition.
Derived from text
Computation; Flux (Rate); Gamma Rays; Lunar Rays; Flux
20050170603 Purdue Univ., West Lafayette, IN, USA
The Crustal Dichotomy and Edge Driven Convection: A Mechanism for Tharsis Rise Volcanism?
King, S. D.; Redmond, H. L.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551;
Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part
of the entire parent document
A vertical wall of constant temperature is a convectively unstable geometry and drives convective motion in the fluid near
the wall. This is the essence of the edge-driven convection hypothesis. On Earth small-scale convection could be triggered
from the vertical step in the thermo-chemical boundary at cratonic keels and continent-ocean boundaries. Seismic evidence
supporting EDC has been observed under the African cratons.
Derived from text
Crusts; Dichotomies; Wall Temperature; Volcanology; Mars Surface
20050170604 Washington Univ., Saint Louis, MO, USA
Mountain Building on Io: An Unsteady Relationship Between Volcanism and Tectonism
Kirchoff, M. R.; McKinnon, W. B.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also
20050170551; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on
CD-ROM only as part of the entire parent document
Introduction: Most mountains on Io are formed through tectonic mechanisms, since few observed seem to be volcanic.
Volcanism may still play an important role in mountain formation, however, e.g., as indicated by the now famous degree-2
anticorrelation between mountain and volcano distributions. Three major hypotheses for mountain formation that have been
proposed are a) convection-modified subsidence, which states that burial of older volcanic layers by new ones (subsidence)
creates large, global compressional stresses, which are modified by degree-2 mantle convection resulting in two broad regions

each of compression and relative tension; b) plume-focused subsidence, where subsidence stresses are focused by upwelling
mantle plumes impinging on the base of the crust to produce isolated mountains; and c) thermally-modified subsidence, which
proposes that mountains are formed by a combination of thermal and subsidence stresses, the former created in the crust due
to localized or regional reductions in eruption rates, which cause strong increased conductive heating.
Derived from text
Io; Mountains; Volcanoes; Tectonics; Thermal Stresses
20050170605 Jet Propulsion Lab., California Inst. of Tech., Pasadena, CA, USA
RADAR Reveals Titan Topography
Kirk, R. L.; Callahan, P.; Seu, R.; Lorenz, R. D.; Paganelli, F.; Lopes, R.; Elachi, C.; Lunar and Planetary Science XXXVI,
Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original contains black and white illustrations; Copyright; Avail:
CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
The Cassini Titan RADAR Mapper is a K(sub u)-band (13.78 GHz, lambda = 2.17 cm) linear polarized RADAR
instrument capable of operating in synthetic aperture (SAR), scatterometer, altimeter and radiometer modes. During the first
targeted flyby of Titan on 26 October, 2004 (referred to as Ta) observations were made in all modes. Evidence for topographic
relief based on the Ta altimetry and SAR data are presented here. Additional SAR and altimetry observations are planned for
the T3 encounter on 15 February, 2005, but have not been carried out at this writing. Results from the T3 encounter relevant
to topography will be included in our presentation. Data obtained in the Ta encounter include a SAR image swath
Derived from text
Titan; Topography; Synthetic Apertures; Cassini Mission
20050170607 Lunar and Planetary Inst., Houston, TX, USA
MarsLab at the Nevada Test Site: Rover Search for Subsurface Hydrothermal Activity Exposed by Small Craters
Kirkland, L. E.; Herr, K. C.; Adams, P. M.; Prothro, L. B.; Allen, B. M.; Lunar and Planetary Science XXXVI, Part 11; [2005];
2 pp.; In English; See also 20050170551; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy;
Available from CASI on CD-ROM only as part of the entire parent document
373
Hydrothermal alteration products that correlate with ejecta from small craters (less than approx. 100 m deep) could flag
near-surface hydrothermal activity. An accompanying abstract discusses potential airborne (Mars satellite analog) routes to
discover such sites, based on testing from explosion craters at the Nevada Test Site (NTS). Here we report correlated

ground-based studies that use rover-analog, thermal infrared imaging spectroscopy. A primary goal of the airborne study is to
determine routes to discovery of hydrothermal activity on Mars. The goals of the ground-based study are: (1) determine which
materials and textures cause the observed airborne signatures, and which materials are imperceptible; (2) compare the airborne
results to detailed geologic maps; and (3) develop lessons-learned for Mars.
Author
Thermal Mapping; Craters; Infrared Imagery; Mars Surface
20050170608 Lunar and Planetary Inst., Houston, TX, USA
The Search for Underground Hydrothermal Activity Using Small Craters: An Example from the Nevada Test Site
Kirkland, L. E.; Herr, K. C.; Adams, P. M.; Prothro, L. B.; Allen, B. M.; Lunar and Planetary Science XXXVI, Part 11; [2005];
2 pp.; In English; See also 20050170551; Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy;
Available from CASI on CD-ROM only as part of the entire parent document
Summary: Craters can create windows into subsurface geology. Hydrothermal alteration products that correlate with
ejecta from small craters (less than 100 m deep) can flag possible near-surface hydrothermal activity. A region with such
activity is a highly prized target for Mars exploration. Here we describe an airborne (satellite analog) study that identified
mineral indicators of hydrothermal activity exposed by manmade explosion craters in a basalt flow. Abstract presents the
related ground-based study. This field development work draws mainly on operational expertise from outside NASA. One goal
is to develop an operational foundation for routes to discovery for Mars.
Author
Mars Exploration; Hydrothermal Systems; Craters; Basalt
20050170609 NASA Goddard Space Flight Center, Greenbelt, MD, USA
Antipodal Magnetic Anomalies on the Moon, Contributions from Impact Induced Currents Due to Positive Holes and
Flexoelectric Phenomina and Dynamo
Kletetschka, G.; Freund, F.; Wasilewski, P. J.; Mikula, V.; Kohout, Tomas; Lunar and Planetary Science XXXVI, Part 11;
[2005]; 1 pp.; In English; See also 20050170551; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on
CD-ROM only as part of the entire parent document
Large impacts on the Moon generate large pressure pulses that penetrate the whole body. Several of these large impacts
may have generated antipodal structure with anomalous magnetic intensity.These regions can be more than a thousand km
across, with fields of the order of tens to hundreds of nT. This is the case of Orientale, Imbrium, Serenitatis, Crisium, and

Nectaris impact basins. The production of large-scale magnetic fields and associated crustal magnetization due to lunar
basin-forming impacts was hypothesized to have an origin in fields external to the impact plasma cloud that are produced by
the magnetohydrodynamic interaction of the cloud with ambient magnetic fields and plasmas. During the period of
compressed antipodal field amplification, seismic compressional waves from the impact converge at the antipode resulting in
transient shock pressures that reach 2 GPa (20 kbar). This can produce conditions for shock magnetic acquisition of the crust
antipodal to impact basins.
Derived from text
Magnetic Anomalies; Moon; Structural Basins; Transient Pressures; Magnetization
20050170611 NASA Johnson Space Center, Houston, TX, USA
MIMOS II on MER One Year of Mossbauer Spectroscopy on the Surface of Mars: From Jarosite at Meridiani Planum
to Goethite at Gusev Crater
Klingelhoefer, G.; Rodionov, D. S.; Morris, R. V.; Schroeder, C.; deSouza, P. A.; Ming, D. W.; Yen, A. S.; Bernhardt, B.; Renz,
F.; Fleischer, I., et al.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551;
Original contains color illustrations
Contract(s)/Grant(s): DLR-50QM99022; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as
part of the entire parent document
The miniaturized Mossbauer (MB) spectrometer MIMOS II [1] is part of the Athena payload of NASA s twin Mars
Exploration Rovers ‘Spirit’ (MER-A) and ‘Opportunity’ (MER-B). It determines the Fe-bearing mineralogy of Martian soils
and rocks at the Rovers respective landing sites, Gusev crater and Meridiani Planum. Both spectrometers performed
374
successfully during first year of operation. Total integration time is about 49 days for MERA (79 samples) and 34 days for
MER-B (85 samples). For curiosity it might be interesting to mention that the total odometry of the oscillating part of the MB
drive exceeds 35 km for both rovers.
Derived from text
Miniaturization; Payloads; Roving Vehicles; Mars Exploration; Landing Sites; Craters
20050170612 Arizona State Univ., Tempe, AZ, USA
Rock Around the World: Extending a Global Reach to Involve Students in Science Using Infrared Research at Mars
Klug, S. L.; Christensen, P. R.; Rogers, L.; Gorelick, N.; Rogers, D.; Jones, B.; Brindley, T.; Rogers, T.; Ki, J.; Staley, L., et
al.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551; Copyright; Avail: CASI;

A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
The Rock Around the World Program (RATW) began with a blending of desired outcomes from two disciplines - science
and education. First, as an extension of the ASU Mars Education Program, there was a desire to inspire students to become
more interested in science. The premise was that kids of all ages like space and, in turn, kids like Mars. Using the lure of Mars
to get them interested in science seemed like a good plan. Secondly, there was a desire from the ASU Mars science team to
collect more rock samples from around the world to expand the earth-based rock library at Arizona State University. This
library currently supports research that is being conducted by the Thermal Emission Spectrometer (TES), the Thermal
Emission Imaging System (THEMIS) - both in orbit around Mars, and the two Mini-Thermal Emission Spectrometer
(Mini-TES) instruments onboard the Mars Exploration Rovers on the surface of Mars. All of these instruments are currently
being used to study rocks on Mars. The Rock Around the World Program evolved from these beginning ideas and has become
an inspiration to all involved.
Derived from text
Infrared Radiation; Mars Exploration; Mars Surface; Education
20050170613 European Space Agency. European Space Research and Technology Center, ESTEC, Noordwijk, Netherlands
The ESA Exploration Programme: Exomars and Beyond
Kminek, G.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 1 pp.; In English; See also 20050170551; Copyright;
Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
The countries participating in the European Exploration Programme Aurora have recently confirmed and increased their
contribution. The ESA Council has later approved the Agency s budgets for 2005, including the budget for Aurora. These
developments enable major industrial activities to continue in line with original plans. These include work on the ExoMars
mission and the Mars Sample Return mission, in-orbit assembly, rendezvous and docking, habitation and life support systems
plus a broad range of technology development work. The Aurora Exploration Programme has been integrated into the Human
Spaceflight and Microgravity Directorate , which now forms the Human Spaceflight, Microgravity, and Exploration
Directorate of ESA.
Derived from text
European Space Agency; Mars Sample Return Missions; Life Support Systems; Space Flight; Orbital Rendezvous;
Microgravity
20050170614 Tokyo Inst. of Tech., Tokyo, Japan
Presolar Silicate Grains from Primitive Carbonaceous Chondrites Y-81025, ALHA 77307, Adelaide and Acfer 094

Kobayashi, S.; Tonotani, A.; Sakamoto, N.; Nagashima, K.; Yurimoto, H.; Krot, A. N.; Lunar and Planetary Science XXXVI,
Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original contains black and white illustrations; Copyright; Avail:
CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
Recently presolar silicates were found in a few meteorites, Acfer 094 (ungrouped type 3), NWA 530 (CR2), Bishunpur
(LL3.1) and Semarkona (LL3.0). Acfer 094 which is thought to be the most pristine chondrite represents the highest
abundance of approximately 40, 30 and 110 ppm. Some researchers suggest that there are some effects of alteration and
metamorphism in matrix even in the petrologic subtype 3.0 chondrites. Therefore, it is unclear for the effect of alteration and
metamorphism against the submicron order of presolar silicates even in type-3 chondrites. In this study we report the presolar
silicates from the least altered and metamorphosed carbonaceous chondrites, Y-81025 (CO3.0), ALHA 77307 (CO3.0),
Adelaide (ungrouped, linked to CV-CO) and Acfer 094 (ungrouped, linked to CO-CM), which there are some agreement that
the above chondrites are one of the most pristine chondrites.
Derived from text
Carbonaceous Chondrites; Silicates; Metamorphism (Geology); Granular Materials
375
20050170615 Japan Aerospace Exploration Agency, Ibaraki, Japan
Mare Volcanism on the Moon Inferred from Clementine UVVIS Data
Kodama, S.; Yamaguchi, Y.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551;
Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part
of the entire parent document
The compositional distribution and the stratigraphy of the mare basalts are important to our understanding of the
composition of the lunar interior and its thermal evolution. Previous works using the Earth-based telescopes or remote sensing
data revealed a large variation in the composition of mare basalts, and suggested that the basin-scale mare volcanism evolved
independently of neighboring regions. It is therefore necessary to know the chemical properties of mare basalts, together with
their detailed distribution and stratigraphy in each region, and to understand how the mare volcanism evolved compositionally
and spatially in a basin. For these purpose, we have mapped the mare basalts on the nearside of the Moon using the Clementine
UVVIS multi-spectral images, and construct their stratigraphy. This paper presents the result of Oceanus Procellarum and
Mare Imbrium, and discusses the temporal and spatial variations of the mare volcanism of this area and the eastern nearside
region.

Author (revised)
Clementine Spacecraft; Lunar Maria; Moon; Volcanology; Ultraviolet Radiation; Light (Visible Radiation)
20050170616 Jet Propulsion Lab., California Inst. of Tech., Pasadena, CA, USA
Public Outreach and Archiving of Data from the High Resolution Stereo Camera Onboard Mars Express: 2004 The
First Year
Koehler, U.; Neukum, G.; Gasselt, S. v.; Jaumann, R.; Roatsch, Th.; Hoffmann, H.; Zender, J.; Acton, C.; Drigani, F.; Lunar
and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original contains color illustrations;
Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
During the first year of operation, corresponding to the calendar year 2004, the HRSC imaging experiment onboard ESA’s
Mars Express mission recorded 23 Gigabyte of 8-bit compressed raw data. After processing, the amount of data increased to
more than 344 Gigabyte of decompressed and radiometrically calibrated scientifically useable image products. Every six
months these HRSC Level 2 data are fed into ESA’s Planetary Science Archive (PSA) that sends all data also to the Planetary
Data System (PDS) to ensure easy availability to the interested user. On their respective web portals, the European Space
Agency published in cooperation with the Principal Investigator-Group at Freie Universitat Berlin and the German Space
Agency (DLR) almost 40 sets of high-level image scenes and movies for PR needs that have been electronically visited many
hundred thousand times.
Derived from text
Cameras; High Resolution; Mars Express; Stereophotography; Data Processing
20050170617 NASA Goddard Space Flight Center, Greenbelt, MD, USA
Determination of Meteorite Porosity Using Liquid Nitrogen
Kohout, T.; Kletetschka, G.; Pesonen, L. J.; Wasilewski, P. J.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 1 pp.;
In English; See also 20050170551; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part
of the entire parent document
We introduce a new harmless method for porosity measurement suitable for meteorite samples. The method is a
modification of the traditional Archimedean method based on immersion of the samples in a liquid medium like water or
organic liquids. In our case we used liquid nitrogen for its chemically inert characteristics.
Derived from text
Liquid Nitrogen; Meteorites; Porosity

20050170618 Tokyo Univ., Japan
Crystallization Experiment of Los Angeles Basaltic Shergottite: Implication for the Crystallization of Los Angeles and
Dhofar 378
Koizumi, E.; Mikouchi, T.; Chokai, J.; Miyamoto, M.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In
English; See also 20050170551; Original contains black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy;
Available from CASI on CD-ROM only as part of the entire parent document
Los Angeles (LA) is a coarse grained basaltic shergottite composed of pyroxene and maskelynite. Pyroxenes in this
meteorite are pigeonite and augite, and both pyroxenes are extensively zoned from relatively Mg-rich cores to Ferich rims.
376
The Ca zoning pattern is complex and pigeonite and augite are irregularly distributed unlike other basaltic shergottites.
Previous study interpreted this irregular zoning as the result of exsolution at low temperature. Because LA has high plagioclase
abundance similar to QUE94201, there is a possibility that the LA bulk composition represents a parent melt composition.
However, these two shergottites show distinct pyroxene zoning patterns although their compositions are generally similar. In
this study, we performed a crystallization experiment using the LA bulk composition to investigate the crystallization history
of LA. We also compared LA mineralogy with that of Dhofar 378 (DHO) which shows a lot of mineralogical characteristics
similar to LA, and applied the experimental result to explain the differences between LA and DHO.
Derived from text
Basalt; Crystallization; Mineralogy; Shergottites; California
20050170619 Arizona State Univ., Tempe, AZ, USA
Chasmata of Planum Australe, Mars: Are Their Formation and Location Structurally Controlled?
Kolb, E. J.; Tanaka, K. L.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551;
Original contains color illustrations; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part
of the entire parent document
The chasmata within Mars south pole ice cap of Planum Australe are indicators of large-scale erosional episodes that have
resulted in the removal of greater than kilometer-thick stacks of south polar layered deposits (SPLD). Geologic mapping of
a large trough system located between two of the chasmata indicates that the trough’s location and erosional morphologies
are in large part, structurally controlled by SPLD bedding attitudes. The scarps of Promethei and Ultimum Chasma also reveal
dipping SPLD beds. Therefore, to what degree is the location of these chasmata and their formation history controlled by

SPLD bedding and (or) substrate topography? We have undertaken a detailed geologic mapping study of the chasmata using
Mars Global Surveyor (MGS) and Mars Odyssey (MO) datasets to determine their bedding features, formation mechanisms,
and emplacement timing. Syntheses of these observations allow discrimination and characterization of potential structural
controls over chasma formation. This study is part of our 1:1.5M-scale geologic mapping project of Mars north and south polar
ice deposits. A general review of the mapping results is included.
Derived from text
Mars Surface; Planetary Geology; Topography; Plains
20050170621 Washington Univ., Saint Louis, MO, USA
Compositions of Three Lunar Meteorites: Meteorite Hills 01210, Northeast Africa 001, and Northwest Africa 3136
Korotev, R. L.; Irving, A. J.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551;
Original contains color illustrations
Contract(s)/Grant(s): NNG04GG10G; Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as
part of the entire parent document
We report on compositions obtained by instrumental neutron activation analysis on three new lunar meteorites, MET
01210 (Meteorite Hills, Antarctica; 23 g), NEA 001 (Northeast Africa, Sudan; 262 g), and NWA 3136 (Northwest Africa,
Algeria or Morocco; 95 g). As in previous similar studies, we divided our samples into many (8-9) small (approximately 30
mg) subsamples prior to analysis.
Derived from text
Africa; Lunar Surface; Meteoritic Composition
20050170622 Oulu Univ., Finland
Anomalous Depressions on the Circum-Hellas Crater Floors as Seen in the First Year MEX HRSC Images
Korteniemi, J.; Lahtela, H.; Raitala, J.; Neukum, G.; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English;
See also 20050170551; Original contains color and black and white illustrations; Copyright; Avail: CASI;
A01, Hardcopy;
Available from CASI on CD-ROM only as part of the entire parent document
The surface of Mars is divided into smooth northern lowlands and cratered southern highlands. The cratering record
indicates the age of the surface, while the original morphology of individual craters hints to the target material. Furthermore,
craters provide a natural basin for later deposits, thus showing glimpses of the regional evolution. The 2000 km Hellas impact
basin dominates about half of the southern hemisphere of Mars. The region has numerous volcanic, tectonic, glacial, fluvial

and aeolian features, as well as a multitude of large and small impact craters. Fresh large (greater than 5 km) Martian craters
have typically raised rims, a central peak and/or a peak ring and a generally flat floor with slumping on the inner walls. The
additional central or summit pits are common features on Martian craters, and generally related to high volatile content of the
377
target material. These features are subsequently modified and smoothened by later geological processes characteristical for the
area, e.g. erosion, sedimentation and impact cratering. One type of post-impact modification is the creation of depressions on
the crater floor. Such features include pits, large scale fractures and, in some cases, more complex depressions such as
honeycomb-like ridges with intervening pits. Continuing our study of these anomalous crater floors, we map the structures in
the Hellas region using the High Resolution Stereo Color (HRSC) images obtained in 2004. HRSC provides multiple channels
and improved accuracy (10-60m/pix) compared to the previous data sets with related areal coverage.
Derived from text
High Resolution; Mars Craters; Mars Surface; Stereophotography; Anomalies; Structural Basins; Mars Volcanoes
20050170623 Planetary Science Inst., Tucson, AZ, USA
The Fate of Neptune’s Primordial Trojan Companions Lost During Planetary Migration
Kortenkamp, Steve; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551;
Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
An earlier paper (Kortenkamp et al. 2004) investigated the survivability of Trojan type companions of Neptune during
primordial radial migration of the giant planets Jupiter, Saturn, Uranus, and Neptune. A standard planet migration model was
used in which the migration speed decreases exponentially with a characteristic time scale. A series of numerical simulations
were performed, each involving the migrating giant planets plus 1000 test particle Neptune Trojans with initial distributions
of orbital eccentricity, inclination, and libration amplitude similar to those of the known jovian Trojans asteroids. The
simulations were analyzed to measure the survivability of Neptune’s Trojans as a function of migration rate. The results of
this analysis are summarized in this paper.
Derived from text
Asteroids; Gas Giant Planets; Planetary Geology; Neptune (Planet)
20050170628 Hokkaido Univ., Sapporo, Japan
Chaotic Occurrence of Some Deep Moonquakes
Koyama, Junji; Lunar and Planetary Science XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original
contains color illustrations; Copyright; Avail: CASI;

A01, Hardcopy; Available from CASI on CD-ROM only as part of the
entire parent document
Seismic observation on the Moon during the Apollo project from 1969 to 1977 discovered tidally induced moonquakes
occurring at depths about halfway to the center of the Moon [1]. Deep moonquakes were characterized by identical waveforms
at a given station observed at near monthly intervals[2]. The identification of these deep moonquakes and also other events
was made by the visual inspection of long-period seismograms, resulting in 12,558 catalogued events [3]. A new computer
analysis of the Apollo lunar seismic data set using a combination of waveform cross-correlation and single-link cluster analysis
[4] revealed that about 60% of the identified and catalogued events are deep moonquakes, and increased the number of
identified deep moonquakes by more than a factor of five. We have applied a simple nonlinear method of Poincare map to time
distribution of events listed in the new catalogue and it reveals previously undetected features of hidden periodic components
on the deep moonquake activity.
Derived from text
Moonquakes; Seismology; Cluster Analysis; Temporal Distribution; Visual Observation
20050170629 Notre Dame Univ., IN, USA
Distinguishing High-Al Mare Basalt Units Using High Resolution Clementine Data
Kramer, Georgiana Y.; Jolliff, Bradley L.; Neal, Clive R.; Kirkland, Laurel; Fessler, Brian; Lunar and Planetary Science
XXXVI, Part 11; [2005]; 2 pp.; In English; See also 20050170551; Original contains color and black and white illustrations;
Copyright; Avail: CASI;
A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document
The Apollo 14 high-Al basalts have a complex petrologic history (see [1]) and unique source, which may be specific to
all high-Al basalts. They are low in Ti, and distinct from other low-Ti mare basalts by their higher alumina content (12 - 15
wt% Al2O3 compared to7-12wt%Al2O3). Other key oxide concentrations include MgO=7-12 wt%, FeO=13-17 wt%,
TiO2=1.5-3 wt%, and incompatible elements 10 to 100 times chondrite, (e.g., Th concentrations are 0.1-3 ppm). Some of the
high-Al basalts are old (\g4 Ga), and the sample data suggests there are at least three and possibly five distinct sources and
episodes of volcanism represented at the Apollo 14 site alone [1]. Exposures of these basalts near the Apollo 14 are likely
masked by ejecta from the Imbrium impact, which is responsible for the formation of the Apollo 14 breccias and post-dates
eruption of the basalts. This suggests that they could be a significant component of ancient basalts that are now buried beneath
378