Abstract—

For the first time, the calculations of the penetration of protons of the undisturbed solar wind into the daytime atmosphere of Mars due to charge exchange in the extended hydrogen corona (Shematovich et al., 2021) are used allowing us to determine self-consistently the sources of suprathermal oxygen atoms, as well as their kinetics and transport. An additional source of hot oxygen atoms—collisions accompanied by the momentum and energy transfer from the flux of precipitating high-energy hydrogen atoms to atomic oxygen in the upper atmosphere of Mars—was included in the Boltzmann kinetic equation, which was solved with the Monte-Carlo kinetic model. As a result, the population of the hot oxygen corona of Mars has been estimated; and it has been shown that the proton aurorae are accompanied by the atmospheric loss of atomic oxygen, which is evaluated within a range of (3.5–5.8) × 10⁷ cm^–2 s^–1. It has been shown that the exosphere becomes populated with a substantial amount of suprathermal oxygen atoms with kinetic energies up to the escape energy, 2 eV. The atomic oxygen loss rate caused by a sporadic source in the Martian atmosphere—the precipitation of energetic neutral atoms of hydrogen (H‑ENAs) during proton aurorae at Mars—was estimated by the self-consistent calculations according to a set of the Monte-Carlo kinetic models. These values turned out be comparable to the atomic oxygen loss supported by a regular source—the exothermic photochemical reactions (Groeller et al., 2014; Jakosky et al., 2018). It is currently supposed that the atmospheric loss of Mars due to the impact of the solar wind plasma and, in particular, the fluxes of precipitating high-energy protons and hydrogen atoms during solar flares and coronal mass ejections may play an important role in the loss of the neutral atmosphere on astronomic time scales (Jakosky et al., 2018).

中文翻译：

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火星质子极光期间原子氧的大气损失

摘要-

由于扩展的氢日冕中的电荷交换（Shematovich 等人，2021），我们首次使用了未受干扰的太阳风的质子穿透到火星白天大气中的计算（Shematovich 等人，2021 年），使我们能够自洽地确定超热氧原子的来源，以及它们的动力学和传输。热氧原子的另一个来源——碰撞伴随着从火星上层大气中沉淀的高能氢原子流向原子氧的动量和能量转移——被包含在玻尔兹曼动力学方程中，该方程用蒙特-卡罗动力学模型。结果，估计了火星热氧日冕的数量；并且已经表明质子极光伴随着大气中原子氧的损失，⁷厘米^–2秒^–1. 已经表明，外逸层充满了大量超热氧原子，其动能高达逃逸能量 2 eV。由火星大气中的一个零星来源引起的原子氧损失率——在火星质子极光期间高能中性氢原子 (H-ENAs) 的沉淀——是根据一组 Monte-卡罗动力学模型。结果证明，这些值与常规来源支持的原子氧损失相当——放热光化学反应（Groeller 等人，2014 年；Jakosky 等人，2018 年）。目前推测，由于太阳风等离子体的影响，火星的大气损失，特别是，