Emission of OI(630 nm) in proton aurora
Emission of OI(630 nm) in proton aurora
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DOI：
10.1029/2000ja002005
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发表时间：
2001-01-01
影响因子：
2.8
通讯作者：
Rich, FJ
中科院分区：
文献类型：
--
作者：
Lummerzheim, D;Galand, M;Rich, FJ
1997年4月11日，加拿大南部和缅因州中部上空出现红色极光，产生了强度为几千瑞利的氧原子（630纳米）辐射，持续了数小时。在此期间，国防气象卫星计划（DMSP）F12卫星两次经过，并且从四个CEDAR光学层析成像设施（COTIF）站点获取了光学数据。DMSP F12粒子光谱仪观测到电子极光南部的质子沉降，能量通量为几毫瓦每平方米。对COTIF光学观测进行层析反演，得到了沿磁子午线的辐射高度剖面。我们利用一个电离层极光模型综合了所有可用数据。我们的分析表明，该模型仅通过质子沉降就能产生所观测到的极光亮度。
A red aurora occurred over southern Canada and central Maine on April 11, 1997, producing a brightness of O I(630 nm) of several Kilorayleighs, which lasted for several hours. Two passes of the Defense Meteorological Satellite Program (DMSP) F12 satellite occurred during this time, and optical data were obtained from four CEDAR Optical Tomographic Imaging Facility (COTIF) sites. The DMSP F12 particle spectrometers observed proton precipitation south of the electron aurora with energy fluxes of several mW m(-2). Tomographic inversion of the COTIF optical observations gives the altitude profile of emissions along a magnetic meridian. We combine all available data using an ionospheric auroral model. Our analysis shows that the model produces the observed auroral brightness from the proton precipitation alone.