Modeling the Enceladus plume–plasma interaction
Modeling the Enceladus plume–plasma interaction
复制标题
模拟土卫二羽流-等离子体相互作用
DOI：
10.1029/2009gl041613
复制
发表时间：
2009
影响因子：
5.2
通讯作者：
F. Bagenal
中科院分区：
文献类型：
--
作者：
B. Fleshman;P. Delamere;F. Bagenal
我们研究了土星的共转等离子体和土卫二的火山羽流之间的化学相互作用。我们使用适用于水基团反应的物理化学模型，在环境等离子体穿过规定的H2O羽流时，会产生一个包裹。流场被假设为围绕以土卫二为中心的导电障碍物的等离子体，并与土星的磁场对齐，与卡西尼磁力计数据一致。我们探讨的物理化学的影响，由于：（1）一个小的人口的热电子，（2）等离子体流减速响应于新鲜离子的拾取，和（3）中性H2O的源速率。该模型证实，电荷交换主导了当地的化学和H3O+主导了土卫二羽流下游的水基团组成。我们还发现，新鲜的皮卡离子的量在很大程度上取决于中性源的强度和持久的人口的热电子的存在。
We investigate the chemical interaction between Saturn's corotating plasma and Enceladus' volcanic plumes. We evolve a parcel of ambient plasma as it passes through a prescribed H2O plume using a physical chemistry model adapted for water‐group reactions. The flow field is assumed to be that of a plasma around an electrically‐conducting obstacle centered on Enceladus and aligned with Saturn's magnetic field, consistent with Cassini magnetometer data. We explore the effects on the physical chemistry due to: (1) a small population of hot electrons, (2) a plasma flow decelerated in response to the pickup of fresh ions, and (3) the source rate of neutral H2O. The model confirms that charge exchange dominates the local chemistry and that H3O+ dominates the water‐group composition downstream of the Enceladus plumes. We also find that the amount of fresh pickup ions depends heavily on both the neutral source strength and on the presence of a persistent population of hot electrons.