Mathematics – Logic
Scientific paper
Apr 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001ssrv...96..105n&link_type=abstract
Space Science Reviews, v. 96, Issue 1/4, p. 105-164 (2001).
Mathematics
Logic
143
Shock Effects, Crystallization Ages, Cosmic Ray Exposure Ages, Ejection Ages, Provenance
Scientific paper
We review the radiometric ages of the 16 currently known Martian meteorites, classified as 11 shergottites (8 basaltic and 3 lherzolitic), 3 nakhlites (clinopyroxenites), Chassigny (a dunite), and the orthopyroxenite ALH84001. The basaltic shergottites represent surface lava flows, the others magmas that solidified at depth. Shock effects correlate with these compositional types, and, in each case, they can be attributed to a single shock event, most likely the meteorite's ejection from Mars. Peak pressures in the range 15 - 45 GPa appear to be a "launch window": shergottites experienced ~30 - 45 GPa, nakhlites ~20 +/- 5 GPa, Chassigny ~35 GPa, and ALH84001 ~35 - 40 GPa. Two meteorites, lherzolitic shergottite Y-793605 and orthopyroxenite ALH84001, are monomict breccias, indicating a two-phase shock history in toto: monomict brecciation at depth in a first impact and later shock metamorphism in a second impact, probably the ejection event. Crystallization ages of shergottites show only two pronounced groups designated S_1 (~175 Myr), including 4 of 6 dated basalts and all 3 lherzolites, and S_2 (330 - 475 Myr), including two basaltic shergottites and probably a third according to preliminary data. Ejection ages of shergottites, defined as the sum of their cosmic ray exposure ages and their terrestrial residence ages, range from the oldest (~20 Myr) to the youngest (~0.7 Myr) values for Martian meteorites. Five groups are distinguished and designated S_Dho (one basalt, ~20 Myr), S_L (two lherzolites of overlapping ejection ages, 3.94 +/- 0.40 Myr and 4.70 +/- 0.50 Myr), S (four basalts and one lherzolite, ~2.7 - 3.1 Myr), S_DaG (two basalts, ~1.25 Myr), and S_E (the youngest basalt, 0.73 +/- 0.15 Myr). Consequently, crystallization age group S_1 includes ejection age groups S_L, S_E and 4 of the 5 members of S, whereas S_2 includes the remaining member of S and one of the two members of S_DaG. Shock effects are different for basalts and lherzolites in group S/S_1. Similarities to the dated meteorite DaG476 suggest that the two shergottites that are not dated yet belong to group S_2. Whether or not S_2 is a single group is unclear at present. If crystallization age group S_1 represents a single ejection event, pre-exposure on the Martian surface is required to account for ejection ages of S_L that are greater than ejection ages of S, whereas secondary breakup in space is required to account for ejection ages of S_E less than those of S. Because one member of crystallization age group S_2 belongs to ejection group S, the maximum number of shergottite ejection events is 6, whereas the minimum number is 2. Crystallization ages of nakhlites and Chassigny are concordant at ~1.3 Gyr. These meteorites also have concordant ejection ages, i.e., they were ejected together in a single event (NC). Shock effects vary within group NC between the nakhlites and Chassigny. The orthopyroxenite ALH84001 is characterized by the oldest crystallization age of ~4.5 Gyr. Its secondary carbonates are ~3.9 Gyr old, an age corresponding to the time of Ar-outgassing from silicates. Carbonate formation appears to have coincided with impact metamorphism, either directly, or indirectly, perhaps via precipitation from a transient impact crater lake. The crystallization age and the ejection age of ALH84001, the second oldest ejection age at 15.0 +/- 0.8 Myr, give evidence for another ejection event (O). Consequently, the total number of ejection events for the 16 Martian meteorites lies in the range 4 - 8. The Martian meteorites indicate that Martian magmatism has been active over most of Martian geologic history, in agreement with the inferred very young ages of flood basalt flows observed in Elysium and Amazonis Planitia with the Mars Orbital Camera (MOC) on the Mars Global Surveyor (MGS). The provenance of the youngest meteorites must be found among the youngest volcanic surfaces on Mars, i.e., in the Tharsis, Amazonis, and Elysium regions.
Bogard Donald D.
Eugster Otto
Greshake Ansgar
Nyquist Larry E.
Shih Chia-You
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