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题名: Ionospheric inversion of the Venus Express radio occultation data observed by Shanghai 25 m and New Norcia 35 m antennas
作者: Zhang, Su-Jun1, 2, 3; Jian, Nian-Chuan1; Li, Jin-Ling1; Ping, Jin-Song4; Chen, Cong-Yan5; Zhang, Ke-Fei6
刊名: RESEARCH IN ASTRONOMY AND ASTROPHYSICS
出版日期: 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
DOI: 10.1088/1674-4527/15/9/012
文章类型: Article
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.
WOS标题词: Science & Technology ; Physical Sciences
类目[WOS]: Astronomy & Astrophysics
研究领域[WOS]: Astronomy & Astrophysics
关键词[WOS]: SOLAR-WIND INTERACTION ; DAYSIDE IONOSPHERE ; NIGHTSIDE IONOSPHERE ; 2-DIMENSIONAL MODEL ; MAGNETIC-FIELDS ; ATMOSPHERE ; TERMINATOR ; IONOPAUSE ; PLASMA ; HOLES
收录类别: SCI
语种: 英语
WOS记录号: WOS:000360555100012
Citation statistics:
内容类型: 期刊论文
URI标识: http://libir.pmo.ac.cn/handle/332002/16022
Appears in Collections:毫米波和亚毫米波技术实验室_期刊论文

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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
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