The effect of solar flares, coronal mass ejections, and solar wind streams on Venus’ 5577 Å oxygen green line
The effect of solar flares, coronal mass ejections, and solar wind streams on Venus’ 5577 Å oxygen green line
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DOI：
10.1016/j.icarus.2014.01.029
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发表时间：
2014-05
期刊：
影响因子：
3.2
通讯作者：
C. Gray;N. Chanover;T. Slanger;K. Molaverdikhani
中科院分区：
文献类型：
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作者：
C. Gray;N. Chanover;T. Slanger;K. Molaverdikhani
2010年12月至2012年7月，我们使用Apache Point Observatory 3.5 m望远镜上的高分辨率天体物理研究联合会Echelle光谱仪观测了太阳耀斑、日冕物质抛射（CME）和太阳风流后的金星5577.3 OOI（1 S-1D）（氧绿色线）夜光发射特征。自2004年以来，我们第一次检测到了绿色线。发射是高度随时间变化的，检测到的最强发射可与先前已知的最亮检测相媲美，并且发生在三种类型的太阳事件中的每一种之后。我们发现最大的发射发生在日冕物质抛射之后，并认为粒子沉淀是绿色线发射的主要贡献者。
We observed the Venusian 5577.3 Å OI (1S–1D) (oxygen green line) nightglow emission feature after solar flares, coronal mass ejections (CMEs), and solar wind streams from December 2010 to July 2012 using the high resolution Astrophysical Research Consortium Echelle Spectrograph on the Apache Point Observatory 3.5 m telescope. For the first time since 2004, we detected the green line. The emission is highly temporally variable, with the strongest emission detected being comparable to the previously known brightest detection, and to occur after each of the three types of solar events. We find the greatest emission occurs after CMEs and suggest that particle precipitation is the main contributor to green line emission.