Japan Geoscience Union Meeting 2015

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Oral

Symbol P (Space and Planetary Sciences) » P-CG Complex & General

[P-CG32] Planetary atmosphere, ionosphere and magnetosphere

Tue. May 26, 2015 11:00 AM - 11:45 AM A03 (APA HOTEL&RESORT TOKYO BAY MAKUHARI)

Convener:*Takeshi Imamura(Japan Aerospace Exploration Agency, Institute of Space and Astronautical Science), Kanako Seki(Solar-Terrestrial Environment Laboratory, Nagoya University), Yukihiro Takahashi(Department of Cosmosciences, Graduate School of Science, Hokkaido University), Yoshiyuki O. Takahashi(Graduate School of Science, Kobe University), Keiichiro Fukazawa(Academic Center for Computing and Media Studies, Kyoto University), Hiromu Nakagawa(Planetary Atmosphere Physics Laboratory, Department of Geophysics, Graduate School of Science, Tohoku University), Chair:Takeshi Imamura(Japan Aerospace Exploration Agency, Institute of Space and Astronautical Science)

11:09 AM - 11:12 AM

[PCG32-P06] 5um spectro-imaging on the Venus dayside

3-min talk in an oral session

*Sakimi KANO1, Naomoto IWAGAMI1, Mayu HOSOUCHI1, Fumiharu SUZUKI1 (1.Department of Earth and Planetary Science, Graduate School of Science, The University of Tokyo)

Keywords:Venus, super-rotation

In the Venus atmosphere, the wind speed increases with height and reaches about 100 m/s at the cloud top, which corresponds to an angular velocity 60 times faster than the rotation of the planet. It is called super-rotation and its generation mechanism is unknown. To investigate atmospheric wave structures in the cloud region (50-70km), which is said to be important as the acceleration region, most studies have used the ultraviolet wavelength to image atmospheric waves at 70 km. Some studies have used the infrared wavelength and analyzed thermal emissions from the nightside to image atmospheric waves at 50 km. We performed infrared spectroscopic measurements using IRTF/CSHELL in May 2014. Our observation aimed at imaging the waves at 60 km and another altitude region simultaneously. We obtained the distributions of cloud height deviation at 60 km by quantifying carbon dioxide absorption in the 1.07um wavelength region. The distributions of cloud temperature at 70 km were also obtained from 5.04um wavelength region. In this presentation, we will show the latter results and discuss the wave structure at 70 km.