Ionospheric inversion of the Venus Express radio occultation data observed by Shanghai 25 m and New Norcia 35 m antennas

	Ionospheric inversion of the Venus Express radio occultation data observed by Shanghai 25 m and New Norcia 35 m antennas
	Zhang, Su-Jun 1,2,3; Jian, Nian-Chuan 1; Li, Jin-Ling 1; Ping, Jin-Song 4; Chen, Cong-Yan 5; Zhang, Ke-Fei 6
刊名	RESEARCH IN ASTRONOMY AND ASTROPHYSICS
	2015-09-01
卷号	15 期号:9 页码:1559-1570
关键词	planets and satellites: terrestrial planets planets and satellites: atmospheres planets and satellites: detection
英文摘要	Electron density profiles of Venus' ionosphere are inverted from the Venus Express (VEX) one-way open-loop radio occultation experiments carried out by the Shanghai 25 m antenna from November 2011 to January 2012 at solar maximum conditions and by the New Norcia 35 m antenna from August 2006 to June 2008 at solar intermediate conditions. The electron density profile (from 110 km to 400 km), retrieved from the X-band egress observation at the Shanghai station, shows a single peak near 147 km with a peak density of about 2 x 1 0(4) c m(-3) at a solar zenith angle of 94 degrees. As a comparison, the VEX radio science (VeRa) observations at the New Norcia station were also examined, including S- and X-band and dual-frequency data in the ingress mode. The results show that the electron density profiles retrieved from the S-band data are more analogous to the dual-frequency data in terms of the profile shape, compared with the X-band data. Generally, the S-band results slightly underestimate the magnitude of the peak density, while the X-band results overestimate it. The discrepancy in the X-band profile is probably due to the relatively larger unmodeled orbital errors. It is also expected that the ionopause height is sensitive to the solar wind dynamical pressure in high and intermediate solar activities, usually in the range of 200-1000 km on the dayside and much higher on the nightside. Structural variations ("bulges" and fluctuations) can be found in the electron density profiles during intermediate solar activity, which may be caused by the interaction of the solar wind with the ionosphere. Considerable ionizations can be observed in Venus' nightside ionosphere, which are unexpected for the Martian nightside ionosphere in most cases.
收录类别	SCI
语种	英语
WOS记录号	WOS:000360555100012
内容类型	期刊论文
源URL	[http://ir.bao.ac.cn/handle/114a11/5598]
专题	国家天文台_月球与深空探测研究部
作者单位	1.Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China 2.Chinese Acad Sci, Key Lab Planetary Sci, Shanghai 200030, Peoples R China 3.Univ Chinese Acad Sci, Beijing 100049, Peoples R China 4.Chinese Acad Sci, Natl Astron Observ, Key Lab Lunar & Deep Space Explorat, Beijing 100012, Peoples R China 5.Southeast Univ, Sch Informat Sci & Engn, Nanjing 210096, Jiangsu, Peoples R China 6.RMIT Univ, Melbourne, Vic 3001, Australia
推荐引用方式 GB/T 7714	Zhang, Su-Jun,Jian, Nian-Chuan,Li, Jin-Ling,et al. Ionospheric inversion of the Venus Express radio occultation data observed by Shanghai 25 m and New Norcia 35 m antennas[J]. RESEARCH IN ASTRONOMY AND ASTROPHYSICS,2015,15(9):1559-1570.
APA	Zhang, Su-Jun,Jian, Nian-Chuan,Li, Jin-Ling,Ping, Jin-Song,Chen, Cong-Yan,&Zhang, Ke-Fei.(2015).Ionospheric inversion of the Venus Express radio occultation data observed by Shanghai 25 m and New Norcia 35 m antennas.RESEARCH IN ASTRONOMY AND ASTROPHYSICS,15(9),1559-1570.
MLA	Zhang, Su-Jun,et al."Ionospheric inversion of the Venus Express radio occultation data observed by Shanghai 25 m and New Norcia 35 m antennas".RESEARCH IN ASTRONOMY AND ASTROPHYSICS 15.9(2015):1559-1570.