Thermal structure of the Venusian atmosphere from the sub-cloud region to the mesosphere as observed by radio occultation

Hiroki Ando, Takeshi Imamura, Silvia Tellmann, Martin Pätzold, Bernd Häusler, Norihiko Sugimoto, Masahiro Takagi, Hideo Sagawa, Sanjay Limaye, Yoshihisa Matsuda, Raj Kumar Choudhary, Maria Antonita

研究成果: Article査読

16 被引用数 (Scopus)

抄録

We present distributions of the zonal-mean temperature and static stability in the Venusian atmosphere obtained from Venus Express and Akatsuki radio occultation profiles penetrating down to an altitude of 40 km. At latitudes equatorward of 75°, static stability derived from the observed temperature profiles is consistent with previous in-situ measurements in that there is a low-stability layer at altitudes of 50–58 km and highly and moderately stratified layers above 58 km and below 50 km, respectively. Meanwhile, at latitudes poleward of 75°, a low-stability layer extends down to 42 km, which has been unreported in analyses of previous measurements. The deep low-stability layer in the polar region cannot be explained by vertical convection in the middle/lower cloud layer, and the present result thus introduces new constraints on the dynamics of the sub-cloud atmosphere. The Venusian atmosphere is in striking contrast to the Earth’s troposphere, which generally has a deeper low-stability layer at low latitudes than at mid- and high latitudes.

本文言語English
論文番号3448
ジャーナルScientific reports
10
1
DOI
出版ステータスPublished - 2020 12月 1

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