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  • Space Transportation and Safety  (5)
  • Water  (5)
  • 2000-2004  (10)
  • 1990-1994
  • 1
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    Initial results from the Mini-TES experiment in Gusev Crater from the Spirit Rover (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-08-07
    Description: The Miniature Thermal Emission Spectrometer (Mini-TES) on Spirit has studied the mineralogy and thermophysical properties at Gusev crater. Undisturbed soil spectra show evidence for minor carbonates and bound water. Rocks are olivinerich basalts with varying degrees of dust and other coatings. Dark-toned soils observed on disturbed surfaces may be derived from rocks and have derived mineralogy (+/-5 to 10%) of 45% pyroxene (20% Ca-rich pyroxene and 25% pigeonite), 40% sodic to intermediate plagioclase, and 15% olivine (forsterite 45% +/-5 to 10). Two spectrally distinct coatings are observed on rocks, a possible indicator of the interaction of water, rock, and airfall dust. Diurnal temperature data indicate particle sizes from 40 to 80 microm in hollows to approximately 0.5 to 3 mm in soils.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Christensen, P R -- Ruff, S W -- Fergason, R L -- Knudson, A T -- Anwar, S -- Arvidson, R E -- Bandfield, J L -- Blaney, D L -- Budney, C -- Calvin, W M -- Glotch, T D -- Golombek, M P -- Gorelick, N -- Graff, T G -- Hamilton, V E -- Hayes, A -- Johnson, J R -- McSween, H Y Jr -- Mehall, G L -- Mehall, L K -- Moersch, J E -- Morris, R V -- Rogers, A D -- Smith, M D -- Squyres, S W -- Wolff, M J -- Wyatt, M B -- New York, N.Y. -- Science. 2004 Aug 6;305(5685):837-42.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Geological Sciences, Arizona State University, Tempe, AZ 85287, USA. phil.christensen@asu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15297667" target="_blank"〉PubMed〈/a〉
    Keywords: Carbonates ; Geologic Sediments ; Interferometry ; Iron Compounds ; Magnesium Compounds ; *Mars ; *Minerals ; Oxides ; Silicates ; Spectrum Analysis ; Temperature ; Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 2
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    Morphology and composition of the surface of Mars: Mars Odyssey THEMIS results (2003)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2003-06-07
    Description: The Thermal Emission Imaging System (THEMIS) on Mars Odyssey has produced infrared to visible wavelength images of the martian surface that show lithologically distinct layers with variable thickness, implying temporal changes in the processes or environments during or after their formation. Kilometer-scale exposures of bedrock are observed; elsewhere airfall dust completely mantles the surface over thousands of square kilometers. Mars has compositional variations at 100-meter scales, for example, an exposure of olivine-rich basalt in the walls of Ganges Chasma. Thermally distinct ejecta facies occur around some craters with variations associated with crater age. Polar observations have identified temporal patches of water frost in the north polar cap. No thermal signatures associated with endogenic heat sources have been identified.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Christensen, Philip R -- Bandfield, Joshua L -- Bell, James F 3rd -- Gorelick, Noel -- Hamilton, Victoria E -- Ivanov, Anton -- Jakosky, Bruce M -- Kieffer, Hugh H -- Lane, Melissa D -- Malin, Michael C -- McConnochie, Timothy -- McEwen, Alfred S -- McSween, Harry Y Jr -- Mehall, Greg L -- Moersch, Jeffery E -- Nealson, Kenneth H -- Rice, James W Jr -- Richardson, Mark I -- Ruff, Steven W -- Smith, Michael D -- Titus, Timothy N -- Wyatt, Michael B -- New York, N.Y. -- Science. 2003 Jun 27;300(5628):2056-61. Epub 2003 Jun 5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Geological Sciences, Arizona State University, Tempe, AZ 85287-6305, USA. phil.christensen@asu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/12791998" target="_blank"〉PubMed〈/a〉
    Keywords: Carbon Dioxide ; Extraterrestrial Environment ; Geologic Sediments ; Geological Phenomena ; Geology ; *Mars ; Seasons ; Temperature ; Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 3
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    Basaltic rocks analyzed by the Spirit Rover in Gusev Crater (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-08-07
    Description: The Spirit landing site in Gusev Crater on Mars contains dark, fine-grained, vesicular rocks interpreted as lavas. Pancam and Mini-Thermal Emission Spectrometer (Mini-TES) spectra suggest that all of these rocks are similar but have variable coatings and dust mantles. Magnified images of brushed and abraded rock surfaces show alteration rinds and veins. Rock interiors contain 〈/=25% megacrysts. Chemical analyses of rocks by the Alpha Particle X-ray Spectrometer are consistent with picritic basalts, containing normative olivine, pyroxenes, plagioclase, and accessory FeTi oxides. Mossbauer, Pancam, and Mini-TES spectra confirm the presence of olivine, magnetite, and probably pyroxene. These basalts extend the known range of rock compositions composing the martian crust.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉McSween, H Y -- Arvidson, R E -- Bell, J F 3rd -- Blaney, D -- Cabrol, N A -- Christensen, P R -- Clark, B C -- Crisp, J A -- Crumpler, L S -- Des Marais, D J -- Farmer, J D -- Gellert, R -- Ghosh, A -- Gorevan, S -- Graff, T -- Grant, J -- Haskin, L A -- Herkenhoff, K E -- Johnson, J R -- Jolliff, B L -- Klingelhoefer, G -- Knudson, A T -- McLennan, S -- Milam, K A -- Moersch, J E -- Morris, R V -- Rieder, R -- Ruff, S W -- De Souza, P A Jr -- Squyres, S W -- Wanke, H -- Wang, A -- Wyatt, M B -- Yen, A -- Zipfel, J -- New York, N.Y. -- Science. 2004 Aug 6;305(5685):842-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996-1410, USA. mcsween@utk.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15297668" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Geologic Sediments ; Iron Compounds ; Magnesium Compounds ; *Mars ; *Minerals ; Oxides ; *Silicates ; Spectroscopy, Mossbauer ; Spectrum Analysis ; Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 4
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    Surficial deposits at Gusev Crater along Spirit Rover traverses (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-08-07
    Description: The Mars Exploration Rover Spirit has traversed a fairly flat, rock-strewn terrain whose surface is shaped primarily by impact events, although some of the landscape has been altered by eolian processes. Impacts ejected basaltic rocks that probably were part of locally formed lava flows from at least 10 meters depth. Some rocks have been textured and/or partially buried by windblown sediments less than 2 millimeters in diameter that concentrate within shallow, partially filled, circular impact depressions referred to as hollows. The terrain traversed during the 90-sol (martian solar day) nominal mission shows no evidence for an ancient lake in Gusev crater.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Grant, J A -- Arvidson, R -- Bell, J F 3rd -- Cabrol, N A -- Carr, M H -- Christensen, P -- Crumpler, L -- Des Marais, D J -- Ehlmann, B L -- Farmer, J -- Golombek, M -- Grant, F D -- Greeley, R -- Herkenhoff, K -- Li, R -- McSween, H Y -- Ming, D W -- Moersch, J -- Rice, J W Jr -- Ruff, S -- Richter, L -- Squyres, S -- Sullivan, R -- Weitz, C -- New York, N.Y. -- Science. 2004 Aug 6;305(5685):807-10.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20560, USA. grantj@nasm.si.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15297659" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Geologic Sediments ; *Mars ; Minerals ; Silicates ; Volcanic Eruptions ; Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 5
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    Mineralogy at Meridiani Planum from the Mini-TES Experiment on the Opportunity Rover (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-12-04
    Description: The Miniature Thermal Emission Spectrometer (Mini-TES) on Opportunity investigated the mineral abundances and compositions of outcrops, rocks, and soils at Meridiani Planum. Coarse crystalline hematite and olivine-rich basaltic sands were observed as predicted from orbital TES spectroscopy. Outcrops of aqueous origin are composed of 15 to 35% by volume magnesium and calcium sulfates [a high-silica component modeled as a combination of glass, feldspar, and sheet silicates (approximately 20 to 30%)], and hematite; only minor jarosite is identified in Mini-TES spectra. Mini-TES spectra show only a hematite signature in the millimeter-sized spherules. Basaltic materials have more plagioclase than pyroxene, contain olivine, and are similar in inferred mineral composition to basalt mapped from orbit. Bounce rock is dominated by clinopyroxene and is close in inferred mineral composition to the basaltic martian meteorites. Bright wind streak material matches global dust. Waterlain rocks covered by unaltered basaltic sands suggest a change from an aqueous environment to one dominated by physical weathering.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Christensen, P R -- Wyatt, M B -- Glotch, T D -- Rogers, A D -- Anwar, S -- Arvidson, R E -- Bandfield, J L -- Blaney, D L -- Budney, C -- Calvin, W M -- Fallacaro, A -- Fergason, R L -- Gorelick, N -- Graff, T G -- Hamilton, V E -- Hayes, A G -- Johnson, J R -- Knudson, A T -- McSween, H Y Jr -- Mehall, G L -- Mehall, L K -- Moersch, J E -- Morris, R V -- Smith, M D -- Squyres, S W -- Ruff, S W -- Wolff, M J -- New York, N.Y. -- Science. 2004 Dec 3;306(5702):1733-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Geological Sciences, Arizona State University, Tempe, AZ 85287, USA. phil.christensen@asu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15576609" target="_blank"〉PubMed〈/a〉
    Keywords: Calcium Sulfate ; Extraterrestrial Environment ; Ferric Compounds ; Geologic Sediments ; Iron Compounds ; Magnesium Compounds ; Magnesium Sulfate ; *Mars ; *Minerals ; Silicates ; Spacecraft ; Sulfates ; Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 6
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    Quantification Of Fire Signatures For Practical Spacecraft Materials (2003)
    In:  CASI
    Details
    Publication Date: 2018-06-06
    Description: The overall objective of this project is to measure the fire signatures of typical spacecraft materials in 1-g and determine how these signatures may be altered in a microgravity environment. During this project, we will also develop a test technique to obtain representative low-gravity signatures. The specific tasks that will be accomplished to achieve these objectives are to: (1) measure the time history of various fire signatures of typical spacecraft materials in 1-g at varying heating rates, temperatures, convective velocities, and oxygen concentrations, (2) conduct tests in the Zero-Gravity Facility at NASA John H. Glenn Research Center to investigate the manner that a microgravity environment alters the fire signature,(3) compare 0-g and 1-g time histories and determine if 0-g data exhibits the same dependence on the test parameters as experienced in 1-g (4) develop a 1-g test technique by which 0-g fire signatures can be measured. The proposed study seeks to investigate the differences in the identities and relative concentrations of the volatiles produced by pyrolyzing and/or smoldering materials between normal gravity and microgravity environments. Test materials will be representative of typical spacecraft materials and, where possible, will be tested in appropriate geometries. Wire insulation materials of Teflon, polyimide, silicone, and PVC will be evaluated using either cylindrical samples or actual wire insulation. Other materials such as polyurethane, polyimide, melamine, and silicone-based foams will be tested using cylindrical samples, in addition to fabric materials, such as Nomex. Electrical components, such as resistors, capacitors, circuit board will also be tested.
    Keywords: Space Transportation and Safety
    Type: Seventh International Workshop on Microgravity Combustion and Chemically Reacting Systems; 389-392; NASA/CP-2003-212376/REV1
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    NASA TECHNICAL REPORTS
  • 7
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    Evaluation of CO2, N2 and He as Fire Suppression Agents in Microgravity (2004)
    In:  CASI
    Details
    Publication Date: 2018-06-06
    Description: The U.S. modules of the International Space Station use gaseous CO2 as the fire extinguishing agent. This was selected as a result of extensive experience with CO2 as a fire suppressant in terrestrial applications, trade studies on various suppressants, and experiments. The selection of fire suppressants and suppression strategies for NASA s Lunar and Martian exploration missions will be based on the same studies and normal-gravity data unless reduced gravity fire suppression data is obtained. In this study, the suppressant agent concentrations required to extinguish a flame in low velocity convective flows within the 20-sec of low gravity on the KC-135 aircraft were investigated. Suppressant gas mixtures of CO2, N2, and He with the balance being oxygen/nitrogen mixtures with either 21% or 25% O2 were used to suppress flames on a 19-mm diameter PMMA cylinder in reduced gravity. For each of the suppressant mixtures, limiting concentrations were established that would extinguish the flame at any velocity. Similarly, concentrations were established that would not extinguish the flame. The limiting concentrations were generally consistent with previous studies but did suggest that geometry had an effect on the limiting conditions. Between the extinction and non-extinction limits, the suppression characteristics depended on the extinguishing agent, flow velocity, and O2 concentration. The limiting velocity data from the CO2, He, and N2 suppressants were well correlated using an effective mixture enthalpy per mole of O2, indicating that all act via O2 displacement and cooling mechanisms. In reduced gravity, the agent concentration required to suppress the flames increased as the velocity increased, up to approximately 10 cm/s (the maximum velocity evaluated in this experiment). The effective enthalpy required to extinguish flames at velocities of 10 cm/s is approximately the same as the concentrations in normal gravity. A computational study is underway to further evaluate these findings.
    Keywords: Space Transportation and Safety
    Type: Strategic Research to Enable NASA's Exploration Missions Conference and Workshop: Poster Session, Volume 2; 355-363; NASA/CP-2004-213205/VOL2
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  • 8
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    Fire Suppression and Response (2004)
    In:  CASI
    Details
    Publication Date: 2018-06-06
    Description: This report is concerned with the following topics regarding fire suppression:What is the relative effectiveness of candidate suppressants to extinguish a representative fire in reduced gravity, including high-O2 mole fraction, low -pressure environments? What are the relative advantages and disadvantages of physically acting and chemically-acting agents in spacecraft fire suppression? What are the O2 mole fraction and absolute pressure below which a fire cannot exist? What effect does gas-phase radiation play in the overall fire and post-fire environments? Are the candidate suppressants effective to extinguish fires on practical solid fuels? What is required to suppress non-flaming fires (smoldering and deep seated fires) in reduced gravity? How can idealized space experiment results be applied to a practical fire scenario? What is the optimal agent deployment strategy for space fire suppression?
    Keywords: Space Transportation and Safety
    Type: Strategic Research to Enable NASA's Exploration Missions Conference and Workshop: Presentations, Volume 1; 848-862; NASA/CP-2004-213205/VOL1
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  • 9
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    Research Needs in Fire Safety for the Human Exploration and Utilization of Space (2003)
    In:  CASI
    Details
    Publication Date: 2018-06-06
    Description: This viewgraph presentation provides information on developments in spacecraft fire safety research. The presentation includes an overview of the previous Spacecraft Fire Safety Workshop, from 1986, and the influences since then of bioastronautics on combustion science and fire safety. The presentation then gives of overview of the current conference, stating goals and giving a schedule.
    Keywords: Space Transportation and Safety
    Type: Research Needs in Fire Safety for the Human Exploration and Utilization of Space Proceedings and Research Plan; 19-25; NASA/CP-2003-212103
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  • 10
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    Tests of Flammability of Cotton Fabrics and Expected Skin Burns in Microgravity (2004)
    In:  Other Sources
    Details
    Publication Date: 2019-07-18
    Description: During a shuttle launch and other portions of space flight, astronauts wear specialized flame resistant clothing. However during most of their missions on board the Space Shuttle or International Space Station, astronauts wear ordinary clothing, such as cotton shirts and pants. As the behaviour of flames is considerably different in microgravity than under earth's gravity, fabrics are expected to burn in a different fashion in microgravity than when tested on earth. There is interest in determining how this change in burning behaviour may affect times to second and third degree burn of human skin, and how the results of standard fabric flammability tests conducted under earth's gravity correlate with the expected fire behaviour of textiles in microgravity. A new experimental apparatus was developed to fit into the Spacecraft Fire Safety Facility (SFSF), which is used on NASA's KC-135 low gravity aircraft. The new apparatus was designed to be similar to the apparatus used in standard vertical flammability tests of fabrics. However, rather than using a laboratory burner, the apparatus uses a hot wire system to ignite 200 mm high by 80 mm wide fabric specimens. Fabric temperatures are measured using thermocouples and/or an infrared imaging system, while flame spread rates are measured using real time observations or video. Heat flux gauges are placed between 7 and 13 mm away from the fabric specimen, so that heat fluxes from the burning fabric to the skin can be estimated, along with predicted times required to produce skin burns. In November of 2003, this new apparatus was used on the KC-135 aircraft to test cotton and cotton/polyester blend fabric specimens in microgravity. These materials were also been tested using the same apparatus in 1-g, and using a standard vertical flammability test that utilizes a flame. In this presentation, the design of the test apparatus will be briefly described. Examples of results from the KC-135 tests will be provided, including heat fluxes and skin burn predictions. These results will be compared with results from 1-g tests using the same apparatus and a standard fabric flammability test apparatus. Recommendations for future microgravity fabric flammability tests will also be discussed.
    Keywords: Space Transportation and Safety
    Type: Strategic Research to Enable NASA's Exploration Missions Conference; 63; NASA/TM-2004-213114
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