期刊
JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
卷 119, 期 3, 页码 2328-2344出版社
AMER GEOPHYSICAL UNION
DOI: 10.1002/2013JA019221
关键词
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资金
- NASA Goddard Space Flight Center under the Graduate Student Research Program [NNX10AL84H]
- NASA [NNX11AD80G]
- NSF [AST 0908311]
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0908311] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0908472] Funding Source: National Science Foundation
This study uses the Mars Test Particle simulation to create virtual detections of O+, O-2(+), and CO2+ in an orbital configuration in the Mars space environment. These atomic and molecular planetary pickup ions are formed when the solar wind directly interacts with the neutral atmosphere, causing the ions to be accelerated by the background convective electric field. The subsequent ion escape is the subject of great interest, specifically with respect to which species dominates ion loss from Mars. O+ is found to be the dominant escaping ion because of the large sources of transported ions in the low-energy (<10 eV) and high-energy (>1 keV) range. O-2(+) and CO2+ are observed at these energy ranges but with much lower fluxes and are generally only found in the tail between 10 eV and 1 keV. Using individual particle traces, we reveal the origin and trajectories of the low-energy downtail O+ populations and high-energy polar O+ populations that contribute to the total escape. Comparing them against O-2(+) and CO2+ reveals that the extended hot oxygen corona contributes to source regions of high-and low-energy escaping ions. Additionally, we present results for solar minimum and maximum conditions with respect to ion fluxes and energies in order to robustly describe the physical processes controlling planetary ion distributions and atmospheric escape.
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