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Computer Simulation of Sputtering of Lunar Regolith by Solar Wind Protons: Contribution to Change of Surface Composition and to Hydrogen Flux at the Lunar Poles

机译：太阳风质子溅射月go石的计算机模拟：对月球两极表面组成变化和氢通量的贡献

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摘要

A computer simulation of the sputtering of lunar soil by solar wind protons was performed with the TRIM program. The rate of the sputtering-induced erosion of regolith particles was shown to be less than 0.2 A per year. A preferential sputtering of Ca, Mg, and O was found along with a less intense sputtering of Fe, Si, and Ti. However, with no other selection mechanisms, surface concentrations of the atoms would differ from the volume ones by no more than 6%. The enrichment of rims of regolith particles with iron occurs as a result of selective removal of lighter atoms from the lunar surface because of different energies of escape from the Moon's gravity. The energy distributions proved to be the same for all sorts of the sputtered atoms, except for implanted hydrogen; thus, a greater fraction of the atoms left on the lunar surface corresponds to heavier elements. According to simulation results, the concentration of reduced iron observed in the mature regolith could be attained during the time of regolith particle exposure to the present flux of solar wind (10~5 years). Thus, sputtering can provide the concentration of Fe_0 observed in regolith. On periphery of a cloud of impact vapor the temperature is too low for an irreversible selective removal of evaporation products; thus, a meteoritic bombardment contributes to the formation of composition of the rims of regolith particles mainly through enrichment of the rims with elements from the bulk of the particles. The estimates of fluxes of backscattered solar wind protons and of sputtered protons, earlier implanted to the regolith, demonstrated that their contribution to the proton flux near the poles is only 10~4 cm~(-2) s~(-1). This is by two orders of magnitude smaller than the proton flux from the Earth's magnetosphere which is, therefore, the main source of protons for permanently shaded polar craters of the Moon.
机译：利用TRIM程序对太阳风质子溅射月球土壤进行了计算机模拟。溅射引起的硬质合金颗粒侵蚀的速率显示为每年小于0.2A。发现钙，镁和氧优先溅射，而铁，硅和钛的溅射强度较低。但是，在没有其他选择机制的情况下，原子的表面浓度与体积的浓度之差将不超过6％。由于从月球引力中逸出的能量不同，选择性地从月球表面清除了较轻的原子，从而使铁基富集石颗粒的边缘富集。事实证明，除了注入的氢以外，所有种类的溅射原子的能量分布都相同。因此，留在月球表面的大部分原子对应于较重的元素。根据模拟结果，在将重晶石颗粒暴露于目前的太阳风通量（10〜5年）期间，可以达到在成熟的重晶石中观察到的还原铁浓度。因此，溅射可以提供在硬质合金中观察到的Fe_0的浓度。在冲击蒸气云的周围，温度太低，无法选择性地去除蒸发产物；因此，主要通过使轮辋富含来自大部分粒子的元素，陨石轰击有助于形成重碎屑粒子的轮辋的成分。早期注入到雷戈石中的反向散射太阳风质子和溅射质子的通量估计表明，它们对两极附近质子通量的贡献仅为10〜4 cm〜（-2）s〜（-1）。这比来自地球磁层的质子通量小两个数量级，因此，质子通量是月球永久遮蔽的极地环形坑的主要质子来源。

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  • 来源
    《Solar system research》 |2003年第1期|p.36-50|共15页
  • 作者

    L. V. Starukhina;

  • 作者单位

    Astronomical Observatory, Kharkov State University, Sumskaya ul. 35, Kharkov, 61022 Ukraine;

  • 收录信息 美国《科学引文索引》(SCI);
  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类 天文学;
  • 关键词

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