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Influence of the Hot Oxygen Corona on the Satellite Drag in the Earth's Upper Atmosphere

机译：热氧电晕对地球上层大气中卫星阻力的影响

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摘要

Calculation results on the possible influence of the hot oxygen fraction on the satellite drag in the Earth's upper atmosphere on the basis of the previously developed theoretical model of the hot oxygen geo-corona are presented. Calculations have shown that for satellites with orbits above 500 km, the contribution from the corona is extremely important. Even for the energy flux Q_0 = 1 erg cm~(-2) s~(-1), the contribution of the hot oxygen can reach tens of percent; and considering that real energy fluxes are usually higher, one can suggest that for extreme solar events, the contribution of hot oxygen to the atmospheric drag of the satellite will be dominant. For lower altitudes, the contribution of hot oxygen is, to a considerable degree, defined by the solar activity level. The calculations imply that for the daytime polar atmosphere, the change of the solar activity level from F_(10.7) ~ 200 to F_(10.7)~ 70 leads to an increase in the ratio of the hot oxygen partial pressure to the thermal oxygen partial pressure by a factor of almost 30, from 0.85 to 25%. The transition from daytime conditions to nighttime conditions almost does not change the contribution from suprathermal particles. The decrease of the characteristic energy of precipitating particles, i.e., for the case of charged particles with a softer energy spectrum, leads to a noticeable increase of the contribution of the suprathermal fraction, by a factor of 1.5- 2. It has been ascertained that electrons make the main contribution to the formation of the suprathermal fraction; and with the increase of the energy of precipitating electrons, the contribution of hot oxygen to the satellite drag also increases proportionally. Thus, for a typical burst, the contribution of the suprathermal fraction is 30% even at relatively high solar activity F_(10.7) = 135.
机译：根据以前开发的热氧电晕的理论模型，给出了热氧分数对地球高层大气中卫星阻力的可能影响的计算结果。计算表明，对于轨道长度超过500公里的卫星，电晕的贡献极为重要。即使对于能量通量Q_0 = 1 erg cm〜（-2）s〜（-1），热氧的贡献也可以达到百分之几十；并且考虑到实际的能量通量通常更高，可以建议对于极端的太阳事件，热氧对卫星大气阻力的贡献将占主导地位。对于较低的海拔，热氧的贡献在很大程度上取决于太阳活动水平。计算表明，对于白天的极地大气，太阳活动水平从F_（10.7）〜200更改为F_（10.7）〜70，导致热氧分压与热氧分压的比值增加。几乎减少了30倍，从0.85％降至25％。从白天到夜晚的转变几乎不会改变超热粒子的作用。沉淀粒子的特征能量的降低，即，对于带电粒子具有较软的能谱的情况，导致超热部分的贡献显着增加了1.5-2倍。已经确定电子对超热部分的形成起主要作用。随着沉淀电子能量的增加，热氧对卫星阻力的贡献也成比例增加。因此，对于典型的爆发，即使在相对较高的太阳活动F_（10.7）= 135时，超热部分的贡献也为30％。

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  • 来源
    《Solar system research》 |2011年第3期|p.231-239|共9页
  • 作者

    V. I. Shematovich; D. V. Bisikalo; S. Krauss; W. Hausleitner; H. Lammer;

  • 作者单位

    Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia;

    Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia;

    Space Research Institute, Austrian Academy of Sciences, Graz, Austria;

    Space Research Institute, Austrian Academy of Sciences, Graz, Austria;

    Space Research Institute, Austrian Academy of Sciences, Graz, Austria;

  • 收录信息 美国《科学引文索引》(SCI);
  • 原文格式 PDF
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