Japan Geoscience Union Meeting 2016

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International Session (Oral)

Symbol P (Space and Planetary Sciences) » P-PS Planetary Sciences

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

Sun. May 22, 2016 9:00 AM - 10:30 AM A02 (APA HOTEL&RESORT TOKYO BAY MAKUHARI)

Convener:*Jun Kimura(Earth-Life Science Institute, Tokyo Institute of Technology), Masaki Fujimoto(Institite of Space and Astronautical Science, Japan Aerospace Exploration Agency), Yasumasa Kasaba(Dep. Geophysics Graduate School of Science Tohoku University), Sho Sasaki(Department of Earth and Space Sciences, School of Science, Osaka University), Takayuki Tanigawa(School of Medicine, University of Occupational and Environmental Health), Yasuhito Sekine(Department of Earth and Planetary Science, University of Tokyo), Kunio Sayanagi(Atmospheric and Planetary Sciences Department, Hampton University), Steven Vance(Jet Propulsion Laboratory, Caltech), Chair:Shunichi Kamata(Creative Research Institution, Hokkaido University), Masaki Fujimoto(Institite of Space and Astronautical Science, Japan Aerospace Exploration Agency)

9:30 AM - 9:45 AM

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

*Takashi Mikami1, Yasuto TAKAHASHI1, Kiyoshi Kuramoto1,2 (1.Department of Cosmosciences, Graduate School of Science, Hokkaido University, 2.Center for Planetary Sciences, Kobe)

Keywords:Titan, Atmosphere

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]