日本地球惑星科学連合2016年大会

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セッション記号 P (宇宙惑星科学) » P-PS 惑星科学

[P-PS01] Outer Solar System Exploration Today, and Tomorrow

2016年5月22日(日) 09:00 〜 10:30 A02 (アパホテル&リゾート 東京ベイ幕張)

コンビーナ:*木村 淳(東京工業大学地球生命研究所)、藤本 正樹(宇宙航空研究開発機構・宇宙科学研究本部)、笠羽 康正(東北大学大学院 理学研究科 地球物理学専攻)、佐々木 晶(大阪大学大学院理学研究科宇宙地球科学専攻)、谷川 享行(産業医科大学医学部)、関根 康人(東京大学大学院理学系研究科地球惑星科学専攻)、Sayanagi Kunio(Atmospheric and Planetary Sciences Department, Hampton University)、Vance Steven(Jet Propulsion Laboratory, Caltech)、座長:鎌田 俊一(北海道大学　創成研究機構)、藤本 正樹(宇宙航空研究開発機構・宇宙科学研究本部)

09:30 〜 09:45

[PPS01-03] A massive primordial-atmosphere on proto-Titan formed in a gas-starved disk

*三上 峻1、高橋 康人1、倉本 圭1,2 (1.北海道大学理学院宇宙理学専攻、2.惑星科学研究センター)

キーワード：タイタン、大気

Titan is a known as a satellite with a thick atmosphere (1.5 bar at the surface) mainly composed of nitrogen. Although several hypotheses about the origin of atmosphere have been proposed, it remains an open question how and when such a thick atmosphere was generated. According to the recent satellite formation theory [e.g., Canup and Ward 2002], Titan formed within low temperature and pressure disk. We numerically investigate the property of the primordial atmosphere of Titan that grew in such a circum-planetary disk, especially in terms of the atmospheric mass and the blanketing effect. In spite of such a disk condition, Titan could capture a thick atmosphere strongly bounded by gravity, which is mainly composed of nebula gas components. This would cause a significant blanketing effect inducing differentiation of this satellite, and result in keeping the surface temperature high relatively (~200 K). This suggests that an ammonia-rich proto atmosphere could be kept on Titan even after the disk was dissipated. Titan’s current nitrogen would be generated from ammonia in the proto atmosphere by photochemical reaction [Atreya et al., 1978]