Ejection Process of Martian Meteorites from Shock Metamorphism

Details Ejection Process of Martian Meteorites from Shock Metamorphism Ejection Process of Martian Meteorites from Shock Metamorphism

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993metic..28r.402m&link_type=abstract

Meteoritics, vol. 28, no. 3, volume 28, page 402

Other

2

Impacts, Mars, Maskelynite, Shock, Snc Meteorites

Scientific paper

Many meteorites from the Moon, Mars, and asteroid belts have been found on the Earth. But the detailed ejection process from Mars is not yet clearly known. The purpose of this study is to discuss the ejection of SNC meteorites from Mars by applying shock metamorphic data of feldspar and quartz [1-3]. From the following results obtained in terrestrial impact rocks, martian SNC meteorites are considered to be formed mainly by the formation of maskelynite grains and shocked quartz aggregates (Table 1). 1. SNC meteorites are not the fine-grained aggregates but the coarsegrained meteorite that can be found at terrestrial crater walls [1,2]. 2. Higher-density deviation of shocked quartz in the Zagami achondrite could not be found in terrestrial impact craters. The anomalous high data of glassy shocked quartz grains indicate that the Zagami meteorite collided with other fragments in cold cosmic space under abrupt heating and quenching conditions [3]. 3. Large maskelynite (i.e., diaplectic plagioclase-like grains) can be found near the crater wall of terrestrial impact craters. The anomalous data of SNC shocked plagioclases in diaplectic maskelynites indicate that large main maskelynite grains are formed by the primary impact of extra-Martian bodies at the martian surface. Table 1, which appears here in the hard copy, shows the ejection process of the Zagami SNC achondrite from Mars estimated from shock metamorphism. In short, it requires a large impact to form large maskelynite grains and to eject the SNC meteorites by smaller, high-speed, and oblique impacts as coarsegrained blocks without a major change in texture (Table 1). The existence of shocked quartz in the Zagami achondrites indicates collision to form shocked quartz aggregates and to quench abruptly in cold space between Mars and the Earth. These two or three probable formation stages of the SNC meteorites are consistent with dating data of crystallization and impact ages reported by many scientists [4]. References: [1] Miura Y. (1991) Shock Waves, 1, 35-41. [2] Miura Y. (1992) Proc. Shock Waves (Japan), 2, 54-57. [3] Miura Y. et al. (1993) Symp. 18th NIPR Antarctic Meteorites (Tokyo), in press.

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