Solar Wind-Induced Atmospheric Erosion at Mars: First Results from ASPERA-3 on Mars Express

Solar Wind-Induced Atmospheric Erosion at Mars: First Results from ASPERA-3 on Mars Express
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DOI：
10.1126/science.1101860
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发表时间：
2004-09
期刊：
Science
影响因子：
56.9
通讯作者：
R. Lundin;S. Barabash;H. Andersson;M. Holmström;A. Grigoriev;M. Yamauchi;J. Sauvaud;A. Fedorov;E. Budnik;J. Thocaven;D. Winningham;R. Frahm;J. Scherrer;J. Sharber;K. Asamura;H. Hayakawa;A. Coates;D. Linder;C. Curtis;K. Hsieh;B. Sandel;M. Grande;M. Carter;D. Reading;H. Koskinen;E. Kallio;P. Riihela;W. Schmidt;T. Säles;J. Kozyra;N. Krupp;J. Woch;J. Luhmann;S. Mckenna-Lawler;R. Cerulli-Irelli;S. Orsini;M. Maggi;A. Mura;A. Milillo;E. Roelof;D. Williams;S. Livi;P Brandt;P. Wurz;P. Bochsler
R. Lundin;S. Barabash;H. Andersson;M. Holmström;A. Grigoriev;M. Yamauchi;J. Sauvaud;A. Fedorov;E. Budnik;J. Thocaven;D. Winningham;R. Frahm;J. Scherrer;J. Sharber;K. Asamura;H. Hayakawa;A. Coates;D. Linder;C. Curtis;K. Hsieh;B. Sandel;M. Grande;M. Carter;D. Reading;H. Koskinen;E. Kallio;P. Riihela;W. Schmidt;T. Säles;J. Kozyra;N. Krupp;J. Woch;J. Luhmann;S. Mckenna-Lawler;R. Cerulli-Irelli;S. Orsini;M. Maggi;A. Mura;A. Milillo;E. Roelof;D. Williams;S. Livi;P Brandt;P. Wurz;P. Bochsler
中科院分区：
综合性期刊1区
文献类型：
--
作者：
R. Lundin;S. Barabash;H. Andersson;M. Holmström;A. Grigoriev;M. Yamauchi;J. Sauvaud;A. Fedorov;E. Budnik;J. Thocaven;D. Winningham;R. Frahm;J. Scherrer;J. Sharber;K. Asamura;H. Hayakawa;A. Coates;D. Linder;C. Curtis;K. Hsieh;B. Sandel;M. Grande;M. Carter;D. Reading;H. Koskinen;E. Kallio;P. Riihela;W. Schmidt;T. Säles;J. Kozyra;N. Krupp;J. Woch;J. Luhmann;S. Mckenna-Lawler;R. Cerulli-Irelli;S. Orsini;M. Maggi;A. Mura;A. Milillo;E. Roelof;D. Williams;S. Livi;P Brandt;P. Wurz;P. Bochsler

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火星快车航天器上的空间等离子体和高能原子分析仪（ASPERA）发现，太阳风等离子体和加速电离层离子可以一直观察到火星快车近心点，距离太阳面行星表面270公里。这是非常深的电离层，意味着火星上层大气直接暴露于太阳风等离子体强迫。太阳风等离子体的低空穿透和电离层等离子体的电离可能是由于太阳风的不规则性或扰动，火星的磁异常，或两者兼而有之。
The Analyzer of Space Plasma and Energetic Atoms (ASPERA) on board the Mars Express spacecraft found that solar wind plasma and accelerated ionospheric ions may be observed all the way down to the Mars Express pericenter of 270 kilometers above the dayside planetary surface. This is very deep in the ionosphere, implying direct exposure of the martian topside atmosphere to solar wind plasma forcing. The low-altitude penetration of solar wind plasma and the energization of ionospheric plasma may be due to solar wind irregularities or perturbations, to magnetic anomalies at Mars, or both.