Nightside Auroral H+ and O+ outflows versus energy inputs during a geomagnetic storm
Nightside Auroral H+ and O+ outflows versus energy inputs during a geomagnetic storm
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地磁风暴期间夜面极光 H 和 O 流出与能量输入
DOI：
10.1029/2022ja030923
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发表时间：
2022
期刊：
影响因子：
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通讯作者：
R. J.
中科院分区：
文献类型：
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作者：
Zhao;K.;Kistler;L. M.;Lund;E. J.;Nowrouzi;N.;Kitamura;N.;& Strangeway;R. J.
重新校准的FAST/TEAMS数据用于研究1998年9月24日至25日地磁风暴期间夜间极光中O+和H+流出对能量输入的响应，Strangeway等人（2005），https://doi.org/10.1029/2004JA010829研究了同一场地磁风暴。与尖峰相反，坡印亭通量和电子沉淀能量输入在夜侧的相关性不太好，因此可以区分它们对流出的影响。O+流出量与alfv<s:1>波印廷通量（r= 0.71）和软电子沉淀（r= 0.69）均有较强的相关性，而H+流出量仅与电子数通量（r= 0.74）有较好的相关性。这表明，在没有额外波加速度的情况下，极光H+流出量接近其极限通量，而在额外波加速度的作用下，较重的O+离子流出量增加。
The recalibrated FAST/TEAMS data is used to study the response of O+and H+outflow to energy inputs in the nightside aurora during the 24–25 September 1998 geomagnetic storm, the same storm studied by Strangeway et al. (2005), https://doi.org/10.1029/2004JA010829. In contrast to the cusp, the Poynting flux and electron precipitation energy input are not as well correlated on the nightside, so their effects on outflow can be differentiated. The O+outflow shows a strong correlation with both the Alfvénic Poynting flux (r= 0.71) and the soft electron precipitation (r= 0.69), while the H+outflow only correlates well with the electron number flux (r= 0.74). This indicates that the auroral H+outflow is close to its limiting flux without additional wave acceleration, while the outflow for the heavier O+ion is increased by additional wave acceleration.