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

被引：41

作者：

Ando, Hiroki ^{[1
]}

Imamura, Takeshi ^{[2
]}

Tellmann, Silvia ^{[3
]}

Patzold, Martin ^{[3
]}

Hausler, Bernd ^{[4
]}

Sugimoto, Norihiko ^{[5
]}

Takagi, Masahiro ^{[1
]}

Sagawa, Hideo ^{[1
]}

Limaye, Sanjay ^{[6
]}

Matsuda, Yoshihisa ^{[7
]}

Choudhary, Raj Kumar ^{[8
]}

Antonita, Maria ^{[9
]}

机构：

[1] Kyoto Sangyo Univ, Fac Sci, Kyoto, Japan

[2] Univ Tokyo, Dept Complex Sci & Engn, Chiba, Japan

[3] Univ Cologne, Rheinisches Inst Umweltforsch, Abt Planetenforsch, Cologne, Germany

[4] Univ Bundeswehr Munchen, Inst Raumfahrttech & Weltraumnutzung, Neubiberg, Germany

[5] Keio Univ, Res & Educ Ctr Nat Sci, Dept Phys, Yokohama, Kanagawa, Japan

[6] Univ Wisconsin, Madison, WI USA

[7] Tokyo Gakugei Univ, Dept Astron & Earth Sci, Tokyo, Japan

[8] Sarabhai Space Ctr, Space Phys Lab, Vikram Sarabhai Space Ctr, Thiruvananthapuram, Kerala, India

[9] Indian Space Res Org, Bengaluru, India

来源：

SCIENTIFIC REPORTS | 2020年 / 10卷 / 01期

关键词：

VERTICAL STRUCTURE; MIDDLE ATMOSPHERE; VERA ONBOARD; CIRCULATION; EXPRESS; VORTEX; WAVES;

D O I：

10.1038/s41598-020-59278-8

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

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 degrees, 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 degrees, 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.

引用

页数：7

共 39 条

[1] Vertical structure of the axi-asymmetric temperature disturbance in the Venusian polar atmosphere: Comparison between radio occultation measurements and GCM results [J].