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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Dayside and nightside reconnection rates inferred from IMAGE FUV and Super Dual Auroral Radar Network data
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Dayside and nightside reconnection rates inferred from IMAGE FUV and Super Dual Auroral Radar Network data

机译：的光面和阴面重联率推断从图像FUV和超级双极光雷达网络数据

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摘要

The spectrographic imager at 121.8 nm (SI12) of the far ultraviolet (FUV) experiment onboard the IMAGE spacecraft produces global images of the Doppler-shifted Lyman α emission of the proton aurora. This emission is solely due to proton precipitation and is not contaminated by dayglow, allowing us to monitor the auroral oval on the dayside as well as on the nightside. Remote sensing of the polar aurora can be advantageously supplemented by use of ground-based data from the Super Dual Auroral Radar Network (SuperDARN) that monitors the ionospheric convective flow pattern in the polar region. In the present study, the SI12 images are used to determine the location of the open/closed field line boundary and to monitor its movement. The SuperDARN data are then used to compute the ionospheric electric field at the location of the open/closed boundary. The total electric field is then computed along the boundary accounting for its movement via Faraday's law so that the dayside and nightside reconnection voltages can be derived. This procedure is applied to several substorm intervals observed simultaneously with IMAGE FUV and SuperDARN. The dayside reconnection voltage feeds the magnetosphere with open flux, which is later closed by nightside reconnection. The calculated dayside reconnection rate is consistent with the solar wind properties measured by the Geotail, Wind, and ACE satellites. We identify the presence of nightside reconnection due to pseudobreakups taking place during the growth phase. In several cases, we establish that the nightside reconnection rate is maximum at the time of the substorm expansion phase onset or shortly after, reaching ～120 kV, and then slowly returns to undisturbed values of ～30 kV. The flux closure rate can also start intensifying prior to expansion phase onset, producing pseudobreakups.
机译：121.8 nm的光谱成像仪(SI12)远紫外(FUV)实验上图像探测器产生的全球形象Doppler-shifted莱曼α发射的质子极光。降水和不是dayglow污染了,允许我们监视的极光椭圆在阴面的光面以及。可以方便地感应的极光辅以地面数据的使用超级双极光雷达网络(SuperDARN)监测电离层对流模式在极地地区。SI12图像是用来确定的位置打开/关闭边界线和领域监控它的运动。用于计算电离层电场打开/关闭边界的位置。然后计算在总电场通过边界占其运动法拉第定律,这样的光面和阴面重新连接电压可以派生。程序应用于几个亚暴间隔FUV同时观测到的图像和SuperDARN。提要的磁气圈开放通量,后来被阴面重新连接关闭。的光面重联率计算与太阳风属性一致测量Geotail、风能和王牌卫星。由于pseudobreakups发生重新连接在增长阶段。建立阴面重联率最大的亚暴扩张开始阶段或之后不久,达到~ 120千伏,然后慢慢地回到原状的值~ 30千伏。加剧扩张阶段开始之前,生产pseudobreakups。

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