Solar wind effect on the multi-fluid plasma expansion in the Venusian upper ionosphere

被引：0
作者：
Salem, S. [1 ,2 ]
Moslem, W. M. [1 ,3 ,4 ]
Fichtner, H. [1 ]
Lazar, M. [1 ,5 ]
机构：
[1] Ruhr Univ Bochum, Inst Theoret Phys 4, D-44780 Bochum, Germany
[2] Arab Acad Sci & Technol AAST, Coll Engn & Technol, Basic & Appl Sci Dept, Port Said, Egypt
[3] Port Said Univ, Fac Sci, Dept Phys, Port Said 42521, Egypt
[4] British Univ Egypt BUE, Ctr Theoret Phys, El Shorouk City, Cairo, Egypt
[5] Katholieke Univ Leuven, Ctr Math Plasma Astrophys, Dept Math, Celestijnenlaan 200B, B-3001 Leuven, Belgium
来源：
ASTRONOMY & ASTROPHYSICS | 2024年 / 685卷
关键词：
hydrodynamics; plasmas; methods: numerical; solar wind; planets and satellites: atmospheres; DUSTY PLASMA; ESCAPE; IONS; TEMPERATURE; WAVES; FIELD;
D O I：
10.1051/0004-6361/202245773
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Inspired by the observations suggesting that at altitudes of about 1000 km the interaction between solar wind streams and Venus' ionosphere plasma leads to ions acceleration and outflow, the influence of different solar wind physical parameters, such as densities, temperatures and initial streaming velocities, has been studied. The ionosphere plasma system consists of two positive ion populations O+, H+ and electrons along with the solar wind streaming protons and electrons. We calculated the generated oxygen and hydrogen ions flow velocities and the electric fields. In addition, we calculated rough estimates for the escaping flux of ion populations (O+, H+) from Venus' ionosphere and compared them to observations. To a large extent, we found that the estimates match. We also discuss the relevance of ionospheric ion acceleration and outflow from Venus' upper.
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页数：8
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