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The Space Studies Board of the National Research Council (NRC) serves as the primary adviser to the National Aeronautics and Space Administration (NASA) on planetary protection policy, the purpose of which is to preserve conditions for future biological and organic exploration of planets and other solar system objects and to protect Earth and its biosphere from potential extraterrestrial sources of contamination. In October 1995 the NRC received a letter from NASA requesting that the Space Studies Board examine and provide advice on planetary protection issues related to possible sample-return missions to near-Earth solar system bodies.
Shock and thermal metamorphism of meteorites from differentiated bodies such as the Moon and Mars have the potential to disturb chronometric information contained in these meteorites. In order to understand the impact-related mechanisms and extent of disturbance to isochrons, we undertook experiments to shock and heat samples of 10017, a 3.6 billion year old lunar basalt. One sub-sample was shocked to 55 GPa, a second subsample was heated to 1000 C for one week, and a third sub-sample was maintained as a control sample. Of the isotope systems analyzed, the Sm-Nd system was the least disturbed by shock or heat, followed by the Rb-Sr system. Ages represented by the 238U-2°6Pb isotope system were degraded by shock and destroyed with heating. In no case did either shock or heating alone result in rotated or reset isochrons that represent a spurious age. In some cases the true crystallization age of the sample was preserved, and in other cases age information was degraded or destroyed. Although our results show that neither shock nor thermal metamorphism alone can account for the discordant ages represented by different isotope systems in martian meteorites, we postulate that shock metamorphism may render a meteorite more susceptible than unshocked material to subsequent disturbance during impact-related heating or aqueous alteration on Mars or Earth. The combination of these processes may result in the disparate chronometric information preserved in some meteorites.
This book introduces the unusual shock-related mineralogical features of the shocked Suizhou L6 (S5) meteorite. The olivine and pyroxene in Suizhou display a mosaic shock feature, while most of plagioclase grains have transformed to glassy maskelynite. A few of the shock-induced melt veins in the meteorite are the simplest, straightest and thinnest ones among all shock-vein-bearing meteorites, and contain the most abundant high-pressure mineral species. Among the 11 identified species, tuite, xieite, and the post-spinel CF-phase of chromite are new minerals. The meteorite experienced a peak shock pressure up to 24 GPa and temperatures of up to 1000° C. Locally developed shock veins were formed at the same pressure, but at an elevated temperature of about 2000° C that was produced by localized shear-friction stress. The rapid cooling of the extremely thin shock veins is the main reason why 11 shock-induced high-pressure mineral phases could be preserved in them so well. This book offers a helpful guide for meteoritics researchers and mineralogists and invaluable resource for specialists working in high-pressure and high-temperature mineralophysics.
Three thin sections of the Tissint Martian meteorite were examined by an array of in situ techniques in order to assess the possibility that a geochemical signature characteristic of the Martian near-surface has been preserved within the meteorite. Tissint is a recent basaltic Martian fall that contains an abundance of shock-generated melt glass that formed by a variety of mechanisms including grain-boundary frictional melting, concentration of shockwaves along boundaries of minerals with contrasting shock-impedance, and void collapse. Tissint is special amongst the suite of Martian meteorites in that it is only the fifth witnessed Martian fall, and its short residence time in a hot desert precluded significant terrestrial weathering. Shock melt pockets form in situ by local melting of igneous phases. Major element compositions and rare earth element patterns do not suggest a contribution from Martian soil or minerals derived from the Martian surface (e.g. jarosite) to the shock melt. Shock-metamorphic sulfides (iron-sulfide spherules within shock melt pockets) exhibit elevated Fe/S ratios compared to groundmass sulfides that were not incorporated into shock melt pockets or veins. Additionally, Raman spectra collected for shock-metamorphic sulfides exhibit Raman peaks characteristic of hematite. These Raman peaks are not present for groundmass sulfides; sulfides were altered (oxidized) as a consequence of the shock event. Thermal modelling results show that cooling times for individual regions of shock melt are controlled by their size, geometry, proximity to other regions of shock melt, and the presence or absence of vesicles. Volatile abundances determined by SIMS revealed that H2O and Cl concentrations are correlated in shock melt glass. Water, chlorine, and fluorine concentrations are not correlated with phosphorus; water in Tissint shock melt glass cannot be attributed to igneous apatite. Hydrogen isotopes demonstrate that the water within Tissint shock melt glass has experienced mixing between two reservoirs: the Martian mantle and the Martian near-surface. For shock melt glass containing vesicles, the shock melt may partially devolatilize to the vesicle before quenching was complete. A geochemical signature derived from the Martian near-surface is preserved in Tissint shock melt pockets, observed primarily in H2O and Cl concentrations and hydrogen isotopes. This signature is very minor and is only detectable by sensitive techniques. Shock melt pockets with the greatest potential to preserve such a signature are isolated from other regions of shock melt, vesicle-free, and glassy.
30% discount for members of The Mineralogical Society of Britain and Ireland This volume addresses the fundamental factors that underlie our understanding of mineral behaviour and crystal chemistry - a timely topic given current advances in research into the complex behaviour of solids and supercomputing.
A comprehensive summary of the mineralogy of all meteorite groups and the origin of their minerals.
The biological effects of asteroid and comet impacts have been widely viewed as primarily destructive. The role of an impactor in the K/T boundary extinctions has had a particularly important influence on thinking concerning the role of impacts in ecological and biological changes. th During the 10 and final workshop of the ESF IMPACT program during March 2003, we sought to investigate the wider aspects of the involvement of impact events in biological processes, including the beneficial role of these events from the prebiotic through to the ecosystem level. The ESF IMPACT programme (1998-2003) was an interdisciplinary effort that is aimed at understanding impact processes and their effects on the Earth environment, including environmental, geological and biological changes. The IMPACT programme has 15 member states and the activities of the programme range from workshops to short courses on topics such as impact stratigraphy, shock metamorphism, etc. The program has also awarded mobility grants and been involved in the development of teaching aids and numerous publications, including this one.
Organized rock by rock, with brief mention to each important paper according to subject.
Volatiles in the Martian Crust is a vital reference for future missions - including ESA’s EXO Mars and NASA’s Mars2020 rover - looking for evidence of life on Mars and the potential for habitability and human exploration of the Martian crust. Mars science is a rapidly evolving topic with new data returned from the planet on a daily basis. The book presents chapters written by well-established experts who currently focus on the topic, providing the reader with a fresh, up-to-date and accurate view. Organized into two main sections, the first half of the book focuses on the Martian meteorites and specific volatile elements. The second half of the book explores processes and locations on the crust, including what we have learned about volatile mobility in the Martian crust. Coverage includes data from orbiter and in situ rovers and landers, geochemical and geophysical modeling, and combined data from the SNC meteorites. Presents information about the nature, relationship, and reactivity of chemical elements and compounds on Mars Explores the potential habitability of Mars Provides a comprehensive view of volatiles in the Martian crust from studies of actual samples as well as from the variety of landed missions, including the MER and Curiosity rovers Delivers a vital reference for ongoing and future missions to Mars while synthesizing large data sets and research on volatiles in the Martian atmosphere Concludes with an informative summary chapter that looks to future Mars missions and what might be learned