SCIENTIFIC AND TECHNICAL AEROSPACE REPORTS
A Biweekly Publication of the National Aeronautics and Space Administration
VOLUME 44, ISSUE 8 - April 21, 2006
91 LUNAR AND PLANETARY SCIENCE AND EXPLORATION
Includes planetology; selenology; meteorites; comets; and manned and unmanned planetary and lunar flights.
For spacecraft design or space stations see 18 Spacecraft Design, Testing and Performance.
20060010188 California Inst. of Tech., Pasadena, CA, USA
Lunar Seismic Detector to Advance the Search for Strange Quark Matter
Galitzki, Nicholas B.; Summer Student Research Presentations; August 2005, pp. 33; In English; See also 20060010186; NoCopyright; Available from CASI only as part of the entire parent document
Detection of small seismic signals on the Moon are needed to study lunar internal structure and to detect possible signalsfrom Strange Quark m&er transit events. The immediate objective is to create a prototype seismic detector using a tunnel diodeoscillator with a variable capacitor attached to a proof mass. The device is designed to operate effectively on the Moon, whichrequires a low power consumption to operate through lunar night, while preserving sensitivity. The goal is capacitanceresolution of better than 1 part in 10’ and power consumption of less than 1 watt. Author.
Quarks; Signal Detection; Seismic Energy; Moon; Oscillators; Tunnel Diodes; Energy Consumption; Capacitance
20060010191 North Dakota Univ., ND, USA
Miniature Instrumentation for SIPR (Subsurface Ice PRobe)
Ostmo, Karl P.; Summer Student Research Presentations; August 2005, pp. 42; In English; See also 20060010186; NoCopyright; Available from CASI only as part of the entire parent document
Ice coring has proved to be a valuable scientific tool for determining climate history on Earth. The goal of the SIPR projectis to develop a simple extraterrestrial ice sampling method of comparable value to coring. The SIPR probe works by meltingits way through glacial ice, pumping the melt water to the surface for analysis as it descends hundreds of meters. The specificgeometry of the probe, along with size and power constraints, requires creative diagnostic instrumentation. A thin, verticallystrung heated filament will provide continuous-level monitoring of water in down-hole containers. The filament has anappreciable temperature coefficient to resistance (TCR), so as water cools the wire, its resistance decreases. At a constantelectrical current, the voltage across the filament varies linearly with water level. Author
Miniaturization; Probes; Ice; Earth Surface; Measuring Instruments
20060010192 Princeton Univ., NJ, USA
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Analyzing MER Uplink Reports
Savin, Stephen C.; Summer Student Research Presentations; August 2005, pp. 46; In English; See also 20060010186; NoCopyright; Available from CASI only as part of the entire parent document
The MER project includes two rovers working simultaneously on opposite sides of Mars each receiving commands onlyonce a day. Creating this uplink is critical, since a failed uplink means a lost day and a waste of money. Examining the processof creating this uplink, I tracked the use of the system developed for requesting observations as well as the development, fromstage to stage, in forming an activity plan. I found the system for requesting observations was commonly misused, if used atall. There are half a dozen reports to document the creation of the uplink plan and often there are discrepancies among them.Despite this, the uplink process worked very well and MER has been one of the most successful missions for NASA in recentmemory. Still it is clear there is room for improvement. Author
Mars Roving Vehicles; Mars Surface; Uplinking
20060010194 Wofford Coll., Spartanburg, SC, USA
Characterization of an Electroanalytical Instrument Suite Searching for Water and Life on Mars
Bostic, Heidi E.; Summer Student Research Presentations; August 2005, pp. 30; In English; See also 20060010186; NoCopyright; Available from CASI only as part of the entire parent document
Seeking the existence of life on other planets is an essential part of NASA’s research. Our terrestrial experience suggeststhat water is a mandatory resource for life to exist and thrive. However, instruments capable of detecting water at the levelslikely to be present on Mars are lacking. This project tests the possibility of using electrical measurements of soils, at variablefrequencies, as a water detector. Generally, the electrical resistance of soils can be described as a combination of resistanceand capacitance, which can be described by a vector including a magnitude and (phase) angle. By specifically studying theimpedance measurements and phase angles of different types of soil, spiked with varying concentrations of dissolved ions,measurements can be taken to provide an idea of the behavior of dry Martian soils. The presentation will describe theexperimental technique, apparatus and procedures, as well as results conducted to calibrate the instrument and to establishsample preparation protocols.Author
Electrical Measurement; Water; Soils; Mars Surface; Impedance Measurement; Extraterrestrial Life; Detection;Capacitance; Mars (Planet)
20060010211 Wyoming Univ., Laramie, WY, USA
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Solar System Visualization (SSV) Project
Todd, Jessida L.; Summer Student Research Presentations; August 2005, pp. 48; In English; See also 20060010186; No Copyright; Available from CASI only as part of the entire parent document
The Solar System Visualization (SSV) project aims at enhancing scientific and public understanding through visual representations and modeling procedures.
The SSV project’s objectives are to (1) create new visualization technologies, (2) organize science observations and models, and (3) visualize science results and mission Plans.
The SSV project currently supports the Mars Exploration Rovers (MER) mission, the Mars Reconnaissance Orbiter (MRO), and Cassini.
In support of the these missions, the SSV team has produced pan and zoom animations of large mosaics to reveal details of surface features and topography, created 3D animations of science instruments and procedures, formed 3-D anaglyphs from left and right stereo pairs, and animated registered multi-resolution mosaics to provide context for microscopic images. Author
Solar System; Scientific Visualization; Models
20060010215 Idaho Univ., ID, USA
Approach and Instrument Placement Validation
Ator, Danielle; Summer Student Research Presentations; August 2005, pp. 29; In English; See also 20060010186; No Copyright; Available from CASI only as part of the entire parent document
The Mars Exploration Rovers (MER) from the 2003 flight mission represents the state of the art technology for target approach and instrument placement on Mars. It currently takes 3 sols (Martian days) for the rover to place an instrument on a designated rock target that is about 10 to 20 m away. The objective of this project is to provide an experimentally validated single-sol instrument placement capability to future Mars missions. After completing numerous test runs on the Rocky8 rover under various test conditions, it has been observed that lighting conditions, shadow effects, target features and the initial target distance have an effect on the performance and reliability of the tracking software. Additional software validation testing will be conducted in the months to come. Author
Mars Missions; Roving Vehicles; Mars Exploration; Program Verification (Computers); Mars (Planet)
20060010219 College of the Holy Cross, Worcester, MA, USA
Solar System Visualizations
Brown, Alison M.; Summer Student Research Presentations; August 2005, pp. 30; In English; See also 20060010186; No Copyright; Available from CASI only as part of the entire parent document
Solar System Visualization products enable scientists to compare models and measurements in new ways that enhance the scientific discovery process, enhance the information content and understanding of the science results for both science colleagues and the public, and create.visually appealing and intellectually stimulating visualization products. Missions supported include MER, MRO, and Cassini. Image products produced include pan and zoom animations of large mosaics to reveal the details of surface features and topography, animations into registered multi-resolution mosaics to provide context for microscopic images, 3D anaglyphs from left and right stereo pairs, and screen captures from video footage. Specific products include a three-part context animation of the Cassini Enceladus encounter highlighting images from 350 to 4 meter per pixel resolution; Mars Reconnaissance Orbiter screen captures illustrating various instruments during assembly and testing at the Payload Hazardous Servicing Facility at Kennedy Space Center; and an animation of Mars Exploration Rover Opportunity’s ‘Rub al Khali’ panorama where the rover was stuck in the deep fine sand for more than a month. This task creates new visualization products that enable new science results and enhance the public’s understanding of the Solar System and NASA’s missions of exploration. Author
Solar System; Mars Reconnaissance Orbiter; Mars Exploration; Display Devices; Topography
20060010223 Reed Coll., Portland, OR, USA
Stable Isotope Characteristics of Jarosite: The Acidic Aqueous History of Mars
Earl, Lyndsey D.; Summer Student Research Presentations; August 2005, pp. 32; In English; See also 20060010186; No Copyright; Available from CASI only as part of the entire parent document
The Mars Rover Opportunity found jarosite (Na(+) or K(+))Fe3SO4(OH)6 at the Meridiani Planum site. This mineral forms from the evaporation of an aqueous acidic sulfate brine. Oxygen isotope compositions may characterize formation conditions but subsequent isotope exchange may have occurred between the sulfate and hydroxide of jarosite and water. The rate of oxygen isotope exchange depends on the acidity and temperature of the brine, but it has not been investigated in detail. We performed laboratory experiments to determine the rate of oxygen isotope exchange under varying acidities and temperatures to learn more about this process. Barium sulfate samples were precipitated weekly from acidic sodium sulfate brines. The oxygen isotope composition of the precipitated sulfate was obtained using a Finnigan MAT253 Isotope Ratio Mass-Spectrometer. The results show that water was trapped in barium sulfate during precipitation. Trapped water may exchange with sulfate when exposed to high temperatures, thus changing the isotope composition of sulfate and the observed fractionation factor of oxygen isotope exchange between sulfate and water. The results of our research will contribute to the understanding of oxygen isotope exchange rates between water and sulfate under acidic conditions and provide experimental knowledge for the dehydration of barium sulfate samples. Author
Acidity; Roving Vehicles; Sodium Sulfates; Mars Surface; Isotope Separation; Isotope Ratios; Hydroxides; Oxygen Isotopes; Brines
20060010233 Franklin W. Olin Coll. of Engineering, Needham, MA, USA
Equipping an FPGA-Based Mars Rover With an LN-200 IMU
Zola, Nicholas J.; Summer Student Research Presentations; August 2005, pp. 50; In English; See also 20060010186; No Copyright; Available from CASI only as part of the entire parent document
The Mars Exploration Rovers (MER) currently navigating the surface of Mars are outfitted with an advanced stereovision correlation algorithm which allows them to ‘see’ three-dimensionally and autonomously avoid obstac’les in their path. A bottleneck of this system is that it is computationally intense and requires 3 minutes of processing for every correlated image and path choice. Taking advantage of the optimization and reprogrammability of FPGAs, the Mobility Avionics lab has reduced this process to under a second. The lab is demonstrating the advancement with a prototype rover, complete with an LN-200 inertial measurement unit (IMU), which is a flight spare from MER. The LN-200 is a space-grade, six degrees-of-freedom IMU using three fiber-optic gyroscopes and three silicon accelerometers and no moving parts. It has particular power-sequencing needs and communicates with a specialized serial protocol (SDLC over RS-422), requiring specific hardware and software for proper functionality and interfacing with an FPGA. The process of incorporating the LN-200 into the system is described herein. Author
Field-Programmable Gate Arrays; Mars Exploration; Mars Roving Vehicles; Avionics; Inertial Platforms
20060010238 Nebraska Univ., Lincoln, NE, USA
Crewbot Suspension Design
Wood, Nathan A.; Summer Student Research Presentations; August 2005, pp. 49; In English; See also 20060010186; No Copyright; Available from CASI only as part of the entire parent document
Planetary Surface Robot Work Crews (RWC) represent a new class of construction robots for future deployment in planetary exploration. Rovers currently being used for the RWC platform lack the load carrying capabilities required in regular work. Two new rovers, dubbed CrewBots, being designed in JPL’s Planetary Robotics Lab specifically for RWC applications greatly increase the load carrying capabilities of the platform. A major component of the rover design was the design of the rocker type suspension, which increases rover mobility. The design of the suspension for the Crewbots departed from the design of recent rovers. While many previous rovers have used internal bevel gear differentials, the increased load requirements of the Crewbots calls for a more robust system. The solution presented is the use of an external modified three-bar, slider-linkage, rocker-style suspension that increases the moment arm of the differential. The final product is a suspension system capable of supporting the extreme loading cases the RWC platform presents, without consuming a large portion of the Crewbots’ internal space. Author
Suspension Systems (Vehicles); Planetary Surfaces; Robotics; Roving Vehicles
20060010253 Oregon State Univ., OR, USA
Utilizing Radioisotope Power Systems for Human Lunar Exploration
Schreiner, Timothy M.; Summer Student Research Presentations; August 2005, pp. 46; In English; See also 20060010186; No Copyright; Available from CASI only as part of the entire parent document
The Vision for Space Exploration has a goal of sending crewed missions to the lunar surface as early as 2015 and no later than 2020. The use of nuclear power sources could aid in assisting crews in exploring the surface and performing In-Situ Resource Utilization (ISRU) activities. Radioisotope Power Systems (RPS) provide constant sources of electrical power and thermal energy for space applications. RPSs were carried on six of the crewed Apollo missions to power surface science packages, five of which still remain on the lunar surface. Future RPS designs may be able to play a more active role in supporting a long-term human presence. Due to its lower thermal and radiation output, the planned Stirling Radioisotope Generator (SRG) appears particularly attractive for manned applications. The MCNPX particle transport code has been used to model the current SRG design to assess its use in proximity with astronauts operating on the surface. Concepts of mobility and ISRU infrastructure were modeled using MCNPX to analyze the impact of RPSs on crewed mobility systems. Strategies for lowering the radiation dose were studied to determine methods of shielding the crew from the RPSs. Author
Lunar Exploration; Technology Utilization; Space Exploration; Power Transmission; Radioisotope Heat Sources
20060010259 Massachusetts Inst. of Tech., MA, USA
Photometric and Spectral Study of the Saturnian Satellites
Newman, Sarah F.; Summer Student Research Presentations; August 2005, pp. 41; In English; See also 20060010186; No Copyright; Available from CASI only as part of the entire parent document
Photometric and spectra analysis of data from the Cassini Visual and Infrared Mapping Spectrometer (VIMS) has yielded intriguing findings regarding the surface properties of several of the icy Saturnian satellites. Spectral cubes were obtained of these satellites with a wavelength distribution in the IR far more extensive than from any previous observations. Disk-integrated solar phase curves were constructed in several key IR wavelengths that are indicative of key properties of the surface of the body, such as macroscopic roughness, fluffiness (or the porosity of the surface), global albedo and scattering properties of surface particles. Polynomial fits to these phase curves indicate a linear albedo trend of the curvature of the phase functions. Rotational phase functions from Enceladus were found to exhibit a double-peaked sinusoidal curve, which shows larger amplitudes for bands corresponding to water ice and a linear amplitude-albedo trend. These functions indicate regions on the surface of the satellite of more recent geologic activity. In addition, recent images of Enceladus show tectonic features and an absence of impact craters on Southern latitudes which could be indicative of a younger surface. Investigations into the properties of these features using VIMS are underway. Author
Icy Satellites; Photometry; Saturn (Planet); Spectrum Analysis
20060010352 Geological Survey, Menlo Park, CA, USA
Rationale and Operational Plan to Upgrade the U.S. Gravity Database
Hildenbrand, T. G.; Briesacher, A.; Flanagan, G.; Hinze, W. J.; Hittelman, A. M.; January 2002; 18 pp.; In English Report No.(s): PB2006-107649; USGS/OFR-02-463; No Copyright; Avail.: National Technical Information Service (NTIS)
A concerted effort is underway to prepare a substantially upgraded digital gravity anomaly database for the USA and to make this data set and associated usage tools available on the internet. This joint effort, spearheaded by the geophysics groups at the National Imagery and Mapping Agency (NIMA), University of Texas at El Paso (UTEP), U.S. Geological Survey (USGS), and National Oceanic and Atmospheric Administration (NOAA), is an outgrowth of the new geoscientific community initiative called Geoinformatics. This dominantly geospatial initiative reflects the realization by Earth scientists that existing information systems and techniques are inadequate to address the many complex scientific and societal issues. Currently, inadequate standardization and chaotic distribution of geoscience data, inadequate accompanying documentation, and the lack of easy-to-use access tools and computer codes for analysis are major obstacles for scientists, government agencies, and educators. NTIS
Data Bases; Gravitation; Gravity Anomalies
20060010503 Wyle Labs., Inc., Houston, TX, USA
Mitigation Strategies for Acute Radiation Exposure During Space Flight
Hamilton, Douglas R.; Epelman, Slava; January 2006; 2 pp.; In English; Aerospace Medicine Association Annual Conference, 8-12 May 2005, Kansas City, MO, USA; Copyright; Avail.: Other Sources; Abstract Only
AWhile there are many potential risks in a Moon or Mars mission, one of the most important and unpredictable is that of crew radiation exposure. The two forms of radiation that impact a mission far from the protective environment of low-earth orbit, are solar particle events (SPE) and galactic cosmic radiation (GCR). The effects of GCR occur as a long-term cumulative dose that results increased longer-term medical risks such as malignancy and neurological degeneration. Unfortunately, relatively little has been published on the medical management of an acute SPE that could potentially endanger the mission and harm the crew. Reanalysis of the largest SPE in August 1972 revealed that the dose rate was significantly higher than previously stated in the literature. The peak dose rate was 9 cGy h(sup -1) which exceeds the low-dose-rate criteria for 25 hrs (National Council on Radiation Protection) and 16 hrs (United Nations Scientific Committee on the Effects of Atomic Radiation). The bone marrow dose accumulated was 0.8 Gy, which exceeded the 25 and 16 hour criteria and would pose a serious medical risk. Current spacesuits would not provide shielding from the damaging effects for an SPE as large as the 1972 event, as increased shielding from 1-5 gm/cm(sup 2) would do little to shield the bone marrow from exposure. Medical management options for an acute radiation event are discussed based on recommendations from the Department of Homeland Security, Centers for Disease Control and evidence-based scientific literature. The discussion will also consider how to define acute exposure radiation safety limits with respect to exploration-class missions, and to determine the level of care necessary for a crew that may be exposed to an SPE similar to August 1972. Author
Radiation Dosage; Manned Space Flight; Aerospace Medicine
20060010509 NASA Johnson Space Center, Houston, TX, USA
Ar-Ar Ages of Nakhlites Y000593, NWA998, and Nakhla and CRE Age of NWA998
Garrison, D. H.; Bogard, D. D.; January 2006; 3 pp.; In English; Lunar and Planetary Science Conference, 14-18 Mar. 2005, League City, TX, USA; Original contains color and black and white illustrations; Copyright; Avail.: CASI: A01, Hardcopy
The seven known Martian nakhlites are Nakhla, Lafayette, Governador Valadares, and four recent finds from hot and cold deserts: MIL03346 from the Transantarctic Mountains, a paired group from the Yamato Mountains (Y000593, Y000749, and Y000802; 1), and two from Morocco (NWA998 and NWA817; 2). Radiometric ages (Sm-Nd, Rb-Sr, U-Pb, and Ar-Ar) for the first three nakhlites, along with Chassigny, fall in the range of 1.19-1.37 Gyr and may suggest a common formation age (e.g., 3). These meteorites also show very similar cosmic-ray (space) exposure ages, which suggests a single ejection event from Mars (3). The ages for nakhlites are different from those of Martian shergottites, whose radiometric ages vary by nearly a factor of three (approximately 165-475 Myr) and whose space exposure ages vary over a factor of approximately 20 (3). Shergottite ages suggest that multiple locations on the Martian surface have been sampled, whereas nakhlite data imply that only one Mars surface location has been sampled. Because older Martian surfaces are expected to be more abundant, it seems surprising that all nakhlites would represent only one Martian impact event. To address this issue, we are measuring the Ar-39-Ar-40 ages of Y-000593, NWA-998, Nakhla, and MIL-03346, and the space (CRE) exposure age of NWA998. Author
Nakhlites; Geochronology; Igneous Rocks
20060010530 NASA Johnson Space Center, Houston, TX, USA
Early Impact Melting and Space Exposure History of the PAT91501 Lchondrite
Bogard, Donald D.; Garrison, D. H.; Herzog, G. F.; Xue, S.; Klein, J.; Middleton, R.; [2004]; 4 pp.; In English; Lunar and Planetary Science Conference, 14-18 Mar. 2004, League City, TX, USA; Original contains color illustrations; Copyright; Avail.: CASI: A01, Hardcopy
Collisions probably occurred frequently in the early history of the asteroid belt. Their effects, which should be recorded in meteorites, must have included heating and melting along with shock alteration of mineral textures. Some non-chondritic meteorite types e.g., eucrites and IIE and IAB irons - do indeed give evidence of extensive impact heating more than 3.4 Gyr ago. The ordinary chondrites, in contrast, show little evidence of early impact heating. The Ar-Ar and Rb-Sr ages of ordinary chondrites that experienced intense shock are for the most part relatively young, many less than 1.5 Gyr. The numerous L-chondrites with Ar- Ar ages clustering near 0.5 Gy are a well-known example. One of them, the 105-kg Chico Lchondrite, shows the effects of unusually intense heating. It is approximately 60% impact melt and likely formed as a dyke beneath a large crater when the L-chondrite parent body underwent a very large impact approximately 0.5 Gyr ago. In rare instances, older shock dates are indicated for ordinary chondrites. Dixon et al show early impact resetting of Ar-Ar ages of a few LL-chondrites including MIL 99301 at 4.23 0.03 Gyr, but in none of these stones did shock lead to extensive melting. As of 2003, searches for chondritic melts attributable to early shock had turned up only the Shaw L-chondrite, which has an Ar-Ar age of approximately 4.42 Gyr. PAT91501 is an 8.55-kg L-chondrite containing vesicles and metal-troilite nodules. It is a unique, near-total impact melt, unshocked, depleted in siderophile and chalcophile elements, and contains only approximately 10% relic chondritic material. The authors conclude that PAT91501 crystallized rapidly and from a much more homogeneous melt than did Shaw. They suggest that PAT resembles Chico and likely formed as an impact melt vein within an impact crater. To define the history of PAT, we have determined its Ar-39-Ar-40 age and measured several radioactive and stable nuclides produced during its space exposure to cosmic rays. Author
Chondrites; Exposure; Impact Melts; Geochronology; Cosmic Rays
20060011039 NASA Johnson Space Center, Houston, TX, USA
Lunar Sample Compendium
Meyer, Charles; [2005]; 12 pp.; In English; Original contains black and white illustrations; No Copyright; Avail.: CASI: A03, Hardcopy
The purpose of the Lunar Sample Compendium will be to inform scientists, astronauts and the public about the various lunar samples that have been returned from the Moon. This Compendium will be organized rock by rock in the manor of a catalog, but will not be as comprehensive, nor as complete, as the various lunar sample catalogs that are available. Likewise, this Compendium will not duplicate the various excellent books and reviews on the subject of lunar samples (Cadogen 1981, Heiken et al. 1991, Papike et al. 1998, Warren 2003, Eugster 2003). However, it is thought that an online Compendium, such as this, will prove useful to scientists proposing to study individual lunar samples and should help provide backup information for lunar sample displays. This Compendium will allow easy access to the scientific literature by briefly summarizing the significant findings of each rock along with the documentation of where the detailed scientific data are to be found. In general, discussion and interpretation of the results is left to the formal reviews found in the scientific literature. An advantage of this Compendium will be that it can be updated, expanded and corrected as need be. Derived from text
Catalogs (Publications); Lunar Geology; Lunar Rocks; Lunar Soil; Moon
Source: NASA
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