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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Modeling the observed proton aurora and ionospheric convection responses to changes in the IMF clock angle: 1. Persistence of cusp proton aurora
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Modeling the observed proton aurora and ionospheric convection responses to changes in the IMF clock angle: 1. Persistence of cusp proton aurora

机译：模拟观察到的质子极光和电离层对流对IMF时钟角变化的响应：1.尖顶质子极光的持久性

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摘要

We employ a numerical model of cusp ion precipitation and proton aurora emission to fit variations of the peak Doppler-shifted Lyman-α intensity observed on 26 November 2000 by the SI-12 channel of the FUV instrument on the IMAGE satellite. The major features of this event appeared in response to two brief swings of the interplanetary magnetic field (IMF) toward a southward orientation. We reproduce the observed spatial distributions of this emission on newly opened field lines by combining the proton emission model with a model of the response of ionospheric convection. The simulations are based on the observed variations of the solar wind proton temperature and concentration and the interplanetary magnetic field clock angle. They also allow for the efficiency, sampling rate, integration time and spatial resolution of the FUV instrument. The good match (correlation coefficient 0.91, significant at the 98% level) between observed and modeled variations confirms the time constant (～4 min) for the rise and decay of the proton emissions predicted by the model for southward IMF conditions. The implications for the detection of pulsed magnetopause reconnection using proton aurora are discussed for a range of interplanetary conditions.
机译：我们采用了尖峰离子沉淀和质子极光发射的数值模型，以拟合2000年11月26日在IMAGE卫星上FUV仪器的SI-12通道观测到的峰值多普勒频移Lyman-α强度的变化。该事件的主要特征是响应于行星际磁场（IMF）向南定向的两次短暂摆动而出现的。我们通过结合质子发射模型和电离层对流响应模型，在新近打开的场线上重现了这种发射的空间分布。该模拟基于观测到的太阳风质子温度和浓度以及行星际磁场时钟角的变化。它们还考虑了FUV仪器的效率，采样率，积分时间和空间分辨率。观测到的变化与模型变化之间的良好匹配（相关系数0.91，在98％的水平上具有显着性）证实了模型预测的向南IMF条件下质子排放的上升和下降的时间常数（〜4分钟）。讨论了在一系列行星际条件下使用质子极光检测脉冲的绝经重新连接的意义。

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