Japan Geoscience Union Meeting 2014

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International Session (Oral)

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

[P-PS01_30PM2] Toward JUICE and future explorations of outer solar system

Wed. Apr 30, 2014 4:15 PM - 6:00 PM 418 (4F)

Convener:*Jun Kimura(Earth-Life Science Institute, Tokyo Institute of Technology), Takayuki Tanigawa(Institute of Low Temperature Science, Hokkaido University), Sho Sasaki(Department of Earth and Space Sciences, School of Science, Osaka University), Masaki Fujimoto(Institite of Space and Astronautical Science, Japan Aerospace Exploration Agency), Yasumasa Kasaba(Dep. Geophysics Graduate School of Science Tohoku University), Yasuhito Sekine(Department of Complexity Science and Enginerring, Graduate School of Frontier Science, University of Tokyo), Chair:Jun Kimura(Earth-Life Science Institute, Tokyo Institute of Technology), Sho Sasaki(Department of Earth and Space Sciences, School of Science, Osaka University)

5:00 PM - 5:15 PM

[PPS01-10] Simulated radiative forcing by molecules in Jupiter's stratosphere

*Takeshi KURODA1, Alexander MEDVEDEV2, Paul HARTOGH2 (1.Tohoku Univ., 2.MPS)

Keywords:Jupiter, atmospheric radiation, gas giants, JUICE

We present the radiative heating and cooling rates by molecules for Jupiter's upper troposphere and stratosphere (103 to 10-3 hPa) with a newly developed parameterization which is suitable for general circulation models. The scheme is a band model based on the correlated k-distribution approach, which accounts for the 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 band model achieved the accuracy of within 10% in comparison with the line-by-line calculations. We show the sensitivity of the heating/cooling rates due to variations of the mixing ratios of hydrocarbon molecules calculated with this scheme, in addition to the calculated radiative-convective equilibrium temperature which is in agreement with observations in the equatorial region. Our results suggest that the radiative forcing in the upper stratosphere is much stronger than it was thought before [Conrath et al., 1990]. In particular, the characteristic radiative relaxation time decreases exponentially with height from 108 s near the tropopause to 105 s in the upper stratosphere.