Japan Geoscience Union Meeting 2015

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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

Tue. May 26, 2015 12:00 PM - 12:45 PM A03 (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 Complexity Science and Enginerring, Graduate School of Frontier Science, University of Tokyo), kunio Sayanagi(Hampton University), Steven Vance(Jet Propulsion Laboratory, Caltech), Chair:Kunio Sayanagi(Atmospheric and Planetary Sciences Department, Hampton University), Jun Kimura(Earth-Life Science Institute, Tokyo Institute of Technology)

12:30 PM - 12:45 PM

[PPS01-03] Simulation study of Jupiter's stratosphere: development of a new radiation code and impacts on the dynamics

*Takeshi KURODA1, Alexander S. Medvedev2, Jisesh Sethunadh2, Paul Hartogh2 (1.Planetary Plasma and Atmospheric Research Center, Tohoku University, 2.Max Planck Institute for Solar System Research)

Keywords:Jupiter, Stratosphere, Atmospheric radiation, Atmospheric dynamics, Gas giants, JUICE

We have developed a new radiation code of radiative heating and cooling for Jupiter's upper troposphere and stratosphere (103 to 10-3 hPa) suitable for general circulation models (GCMs). It is based on the correlated k-distribution approach, and accounts for all the major radiative mechanisms in the Jovian atmosphere (heating due to absorption of solar radiation by CH4, and cooling in the infrared by C2H6, C2H2, CH4 and collision-induced transitions of H2-H2 and H2-He). The code can be applied for Saturn and extrasolar gas giants. Vertical 1-D calculations using this code demonstrated that temperature of Jupiter's stratosphere is close to radiative-convective equilibrium, and that the radiative relaxation time decreases exponentially with height (from 108 s near the tropopause to 105 s in the upper stratosphere). The latter differs from the study of Conrath et al. (1990), which showed the very long (〜108 s) relaxation time approximately constant throughout the stratosphere. Our calculations with the GCM show that the radiative relaxation time suggested by Conrath et al. (1990) is too long, and cannot sustain convergence of model solutions. With the newly derived vertical profile of relaxation time, simulations converge and produce realistic temperature and wind in Jovian stratosphere.