JpGU-AGU Joint Meeting 2017

Presentation information

[EJ] Poster

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

[P-PS06] [EJ] Results of Venus science with Akatsuki in orbit for 1.5 year

Sat. May 20, 2017 3:30 PM - 5:00 PM Poster Hall (International Exhibition Hall HALL7)

convener:Takehiko Satoh(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency), Takeshi Horinouchi(Faculty of Environmental Earth Science, Hokkaido University), Masaru Yamamoto(Research Institute for Applied Mechanics, Kyushu University), Kevin McGouldrick(University of Colorado Boulder)

[PPS06-P18] Venus nightside infrared spectroscopic study around the 2.3-μm CO2 atmospheric window using IRTF/SpeX data in Jan-Feb 2017

*Yeon Joo Lee1, Hideo Sagawa2, Takao M Sato1, Toru Kouyama3, Javier Peralta1, Eliot Young4, Emmanuel Marcq5, Shigeto Watanabe6, Masataka Imai7, Takeshi Imamura8, Takehiko Satoh1, Masato Nakamura1 (1.ISAS/JAXA, Japan, 2.Kyoto Sangyo Univ., Japan, 3.AIST, Japan, 4.SwRI, U.S.A., 5.LATMOS, France, 6.Hokkaido information Univ., Japan, 7.Hokkaido Univ., Japan, 8.Tokyo Univ., Japan)

Keywords:Venus, Infrared, Spectroscopy, Ground-based observation

Venus has a 96.5% CO2 atmosphere with 20-km thick H2SO4 clouds at 48-70 km altitudes above surface covering the entire planet. The strong CO2 absorption effectively hinder thermal emission from lower atmosphere to space, and the clouds also contribute the opacity. However, there are well-known atmospheric windows which allow us to detect the emission below the clouds. We observed Venus nightside using such a channel around 2.3 μm. The observation was conducted at IRTF, Hawaii, USA, for 15 days in Jan and Feb 2017. As Venus approaches its inferior conjunction in March 2017, the apparent size of Venus increased from 22” to 38” during our observation period. We used a medium resolution spectrometer (SpeX, R~2500 in the 1.68-4.2 μm range), which has sufficient resolving power to study cloud opacity at 48-55 km, as well as spatial distributions of trace gases such as CO, OCS, H2O, SO2 below the clouds at 30-40 km altitudes above surface. This observation was conducted as a coordinated observation with the Japanese Venus mission, Akatsuki, which monitors atmospheric winds and mesospheric SO2 abundance above the clouds. We will compare the trace gaseous spatial distributions below and above the clouds, and investigate their possible correlation.