Space and Planetary Science, Graduate School of Science, University of Tokyo
Remote Sensing Technology Center of Japan(RESTEC)
National Institute of Polar Research
Space and Planetary Science, Graduate School of Science, University of Tokyo
出版者
宇宙航空研究開発機構宇宙科学研究本部
出版者（英）
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)
雑誌名
月・惑星シンポジウム
雑誌名(英)
Proceedings of the ISAS lunar and planetary symposium
巻
42
ページ
26 - 29
発行年
2009-08
会議概要（会議名, 開催地, 会期, 主催者等）
第42回 月・惑星シンポジウム(2009年8月5-7日, 宇宙航空研究開発機構宇宙科学研究本部)
会議概要（会議名, 開催地, 会期, 主催者等）（英）
The 42nd ISAS Lunar and Planetary Symposium (August 5-7, 2009. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)), Sagamihara, Kanagawa Japan
抄録（英）
We developed a model to calculate the cooling rate (or burial depth) by using the Fe-Mg chemical zoning profile of olivine considering diffusional modification during crystal growth, because chemical zoning provides information on thermal history of minerals. We calculated the cooling rate and burial depth of martian meteorites (olivine-phyric shergottites: Yamato980459, DaG476, and EET79001). The calculated cooling rate for an olivine in Yamato980459 is 0.20C/h and that for an olivine in DaG476 is 0.089C/h. The calculated cooling rates for olivines in EET79001 are 0.032C/h, 0.08C/h, and 0.30C/h. This result may be consistent with xenocryst origin of EET79001 olivines. These cooling rates correspond to the burial depth of 2-7 m, assuming the rock-like thermal diffusivity. This result suggests shallow intrusions or lava flows on the surface of Mars for the origin of these shergottites.
The cooling rate of several shergottites as inferred from Fe-Mg zoning of olivine
