Ionospheric effects of solar flares at Mars
Ionospheric effects of solar flares at Mars
复制标题
火星太阳耀斑的电离层效应
DOI：
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发表时间：
2009
期刊：
影响因子：
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通讯作者：
Sachchidanand Singh
中科院分区：
文献类型：
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作者：
K. Mahajan;N. Lodhi;Sachchidanand Singh
通过对火星全球勘测者号上记录的电子密度剖面的分析，我们报告了在火星电离层中一些新的、在高层大气物理学上具有重要意义的太阳耀斑效应的观测结果。我们发现所有耀斑都会导致形成一个明确的E层峰值，这在其他日子里并不总是能看到。此外，虽然大多数耀斑仅导致E区电子密度升高，但一些耀斑会影响E层和F1层。这些与高度相关的效应能够为太阳耀斑期间不同波长波段光子通量的相对增强提供重要信息。利用福克斯（2004年）给出的火星单位光学深度值以及迈耶等人（2002年）的极紫外辐照度模型对巴士底日太阳耀斑进行研究，我们推断明确的E层峰值可能是由10 - 13纳米光谱波段的光子通量增强导致的。这种效应延伸到F1层是由于26 - 91纳米光谱波段变硬，这得到了太阳和太阳风层探测器上的太阳极紫外监测仪测量结果的支持。
From an analysis of electron density profiles recorded aboard Mars Global Surveyor, we report observations of some new and aeronomically important solar flare effects in the ionosphere of Mars. We find that all flares result in the formation of a well defined E layer peak, not always seen on other days. Further, while majority of flares result in elevated electron densities in the E region alone, some flares affect both the E and F1 layers. These altitude ‐ related effects can provide vital information on the relative enhancement of photon fluxes in the various wavelength bands during solar flares. By using the unit optical depth values at Mars from Fox (2004) and the XUV irradiance model of Meier et al. (2002) for the Bastille Day solar flare, we infer that the well defined E peaks could result from enhancement of photon fluxes in the 10–13 nm spectral band. The extension of effect to the F1 layer is due to hardening of the 26–91 nm spectral band, as supported by Solar EUV Monitor measurements on Solar Heliospheric Observatory.