Marsward and tailward ions in the near-Mars magnetotail: MAVEN observations
Marsward and tailward ions in the near-Mars magnetotail: MAVEN observations
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DOI：
10.1002/2015gl065005
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发表时间：
2015-11-16
影响因子：
5.2
通讯作者：
Jakosky, B. M.
中科院分区：
文献类型：
--
作者：
Harada, Y.;Halekas, J. S.;Jakosky, B. M.
我们介绍了火星大气和挥发性演化（MAVEN）观测和火星附近（类似于1-1.5火星半径下游）磁尾的超热（> - 25ev）离子的尾部通量。统计结果表明，马氏质子通量和磁场悬垂模式在上游运动电场方向上有较好的组织。我们观察到显著的马氏质子通量和半球紧密包裹的磁力线指向与上游电场相反的方向。这些特征与在金星上观察到的非常相似。另一方面，氧离子的净通量在火星尾部平均指向尾部，而在金星的同一半球经常观察到向金星方向的氧离子净流量。马斯华质子通量是在氧离子通量存在的情况下产生的，其机制尚不清楚。
We present Mars Atmosphere and Volatile EvolutioN (MAVEN) observations of Marsward and tailward fluxes of suprathermal (>25 eV) ions in the near-Mars (similar to 1-1.5 Mars radii downstream) magnetotail. Statistical results show that the Marsward proton flux and magnetic field draping pattern are well organized by the upstream motional electric field direction. We observe both significant Marsward proton fluxes and tightly wrapped magnetic field lines in the hemisphere pointed in the opposite direction to the upstream electric field. These characteristics are very similar to those observed at Venus. On the other hand, the net flux of oxygen ions points tailward on average in the Martian tail, while net Venusward flows of oxygen ions were observed frequently in the same hemisphere at Venus. The mechanism by which the Marsward proton flux is produced in the presence of tailward oxygen ion flux remains unclear.