Physics
Scientific paper
Jun 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986gecoa..50.1031h&link_type=abstract
(Lunar and Planetary Institute, NASA, American Geophysical Union, et al., Lunar and Planetary Science Conference, 16th, Houston,
Physics
2
Achondrites, Meteoritic Composition, Planetary Evolution, Shock Heating, Thermoluminescence, Mars (Planet), Mineralogy, Recrystallization, Meteorites, Stony Meteorites, Achondrites, Shergotty, Samples, Meteorite, Thermoluminescence, Shock Effects, Heating, Shergottites, Temperature, Minerals, Maskynite, Laboratory Studies, Procedure, Glow Curves, Zagami, Antarctic Meteorites, Alh Meteorites, Alha77005, Eet Meteorites, Eeta79001, Annealing, Crystallization, Cooling, Ejecta, Size, Origin, Source, Mars
Scientific paper
Thermoluminescence (TL) measurements on Shergotty, ALHA 77005, Zagami, and EETA 79001 (lithology A) have been used to obtain further information on the shock history of these meteorites. The level of TL sensitivity in the shergottites varied by a factor of 10, but was always low, probably reflecting the amount of crystalline material in the maskelynite. There are trends in the TL peak temperature, peak width, and TL sensitivity which are believed to be associated with different proportions of feldspar in high- and low-temperature forms. This interpretation is consistent with the observed changes induced in the TL properties by annealing shergottites at 400-900 C. It is suggested that the observed trends were produced during postshock crystallization at a variety of cooling rates, the increasing order of cooling rate being EETA 79001, Zagami, ALHA 77005, and Shergotty, and that there is high-temperature feldspar present in all the samples. This implies a postshock temperature above 600 C, and a small (less than 10 m) size of the ejecta. Current theories are well able to explain how objects of this size could have been ejected from Mars.
Haq Munir
Hasan Fouad A.
Sears Derek W. G.
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