Escape of O(3P), O(1D), and O(1S) from the Martian atmosphere
Escape of O(3P), O(1D), and O(1S) from the Martian atmosphere
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DOI：
10.1016/j.icarus.2017.08.041
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发表时间：
2018-01
期刊：
影响因子：
3.2
通讯作者：
J. Fox;A. Hać
中科院分区：
文献类型：
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作者：
J. Fox;A. Hać
本文计算了在火星热层中，由于O2+的解离复合，在基态和前两个激发亚稳态O(1 D)和O(1 S)中产生的热O原子的逃逸几率、通量和速率。为了将我们的结果与我们以前的计算结果以及其他人的结果进行比较，我们在这里使用了我们以前使用过的Pre-MAVEN模型。为了计算逃逸几率，我们使用了前面描述的蒙特卡罗逃逸程序，但我们在这里首次使用能量相关的弹性截面来计算高能O原子与我们模型中的12个背景物种中的每一个原子的碰撞。我们还引入了三种交换O(3P)和O(1D)原子身份的机制，包括O(3P)到O(1D)的碰撞激发，O(1D)到O(3P)的猝灭，以及O(1D)和O(3P)的激发交换。我们发现，与没有包括这些过程的O原子相比，最初以O(1 D)形式产生的O原子的逃逸几率降低了，但最初以O(3 P)形式产生的O原子的逃逸几率并没有显著降低。作为我们未来研究和其他研究人员的指导，我们在这里综述了有关O原子与其他物种的相互作用的已知情况，在这些相互作用中，O原子的能量发生了变化，以及其他几个热的和逃逸的O的来源，其中许多是其他研究人员提出的。我们将把这些数据纳入未来类似MAVEN的模型中。
We have computed here the escape probabilities, fluxes and rates for hot O atoms that are initially produced in the ground state and the first two excited metastable states, O (1 D) and O (1 S), in the Martian thermosphere by dissociative recombination of O 2+. In order to compare our results with those of our previous calculations and with those of others, we have employed here the pre-MAVEN models that we have used previously. To compute the escape probabilities, we have employed the Monte Carlo escape code that has been described previously, but we here use for the first time energy-dependent elastic cross sections for collisions of the energetic O atoms with each of the twelve background species in our model. We also incorporate three mechanisms that interchange identities of the O (3 P) and O (1 D) atoms, including collisional excitation of O (3 P) to O (1 D), quenching of O (1 D) to O (3 P), and excitation exchange of O (1 D) with O (3 P). We find that the escape probabilities of O atoms that are produced initially as O (1 D) are reduced compared to those in which these processes are not included, but the escape probabilities of O atoms that are initially produced as O (3 P) are not significantly reduced. As a guide for our future research and those of other investigators, we review here what is known about the interactions of O atoms with other species in which the energies of the O atoms are altered, and several other sources of hot and escaping O, many of which have been suggested by other investigators. We will incorporate these data in a future MAVEN-like model.