Japan Geoscience Union Meeting 2014

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International Session (Oral)

Symbol B (Biogeosciences) » B-AO Astrobiology & the Origin of Life

[B-AO01_28AM1] Astrobiology: Origins, Evolution, Distribution of Life

Mon. Apr 28, 2014 9:00 AM - 10:40 AM 502 (5F)

Convener:*Kensei Kobayashi(Department of Chemistry and Biotechnology, Faculty of Engineering, Yokohama National University), Akihiko Yamagishi(Tokyo University of Pharmacy and Life Science, Department of Molecular Biology), Masatoshi Ohishi(Astronomy Data Center, National Astronomical Observatory of Japan), Eiichi Tajika(Department of Complexity Science and Engineering, Graduate School of Frontier Sciences, The University of Tokyo), Takeshi Kakegawa(Graduate School of Science, Tohoku University), Shigeru Ida(Department of Earth and Planetary Science, Graduate School of Science and Technology, Tokyo Institute of Technology), Chair:Masatoshi Ohishi(Astronomy Data Center, National Astronomical Observatory of Japan), Shigeru Ida(Department of Earth and Planetary Science, Graduate School of Science and Technology, Tokyo Institute of Technology)

10:00 AM - 10:25 AM

★ [BAO01-05] Formation of extraterrestrial oceans: Cradles of life

*Sho SASAKI1, Jun KIMURA2, Tadashi KONDO2, Koji MATSUMOTO3, Hiroki SENSHU4, Yasuhito SEKINE5, Takazo SHIBUYA6, Tomoaki KUBO7, Noriyuki NAMIKI4, Yasunori HORI3, Shunichi KAMATA8 (1.Department of Earth and Space Sciences, Osaka University, 2.ELSI, Tokyo Institute of Technology, 3.National Astronomical Observatory, 4.PERC, Chiba Institute of Technology, 5.The University of Tokyo, 6.Japan Agency for Marine-Earth Science and Technology, 7.Department of Earth and Planetary Sciences, Kyushu University, 8.Hokkaido University)

Keywords:icy satellites, habitability, interior ocean, habitable zone, gas giant planets, origin of planetary systems

As one of research groups on "Astrobiology in the Solar System" (a proposal submitted to MEXT), our group will study the origin of icy satellites around giant planets, and the origin and evolution of the interior ocean(s) of those icy bodies and their universality. Outside the so-called snowline of H2O, the mass of protoplanets could be large enough to collect surrounding gas rapidly to form massive gaseous giant planets. Icy satellites would have been formed or trapped by the circumplanetary gas disks around giant planets. In multisatellite cases, orbital resonances may stabilize satellite migration and tidal dissipation would provide heat for sustaining interior oceans. Even when surface temperature is lower at a further distance from the sun, additional ice component (NH3, CH4, CO, etc.) would decrease the melting temperature. As a result, the more extended condition for presence of liquid water can be considered in comparison with the conventional habitable zone (with surface water).