We present detailed analysis of the global relativistic electron dynamics as measured by total radiation belt content (RBC) during coronal mass ejection (CME) and corotating interaction region (CIR)‐driven geomagnetic storms. Recent work has demonstrated that the response of the outer radiation belt is consistent and repeatable during geomagnetic storms. Here we build on this work to show that radiation belt dynamics can be divided into two sequential phases, which have different solar wind dependencies and which when analyzed separately reveal that the radiation belt responds more predictably than if the overall storm response is analyzed as a whole. In terms of RBC, in every storm we analyzed, a phase dominated by loss is followed by a phase dominated by acceleration. Analysis of the RBC during each of these phases demonstrates that they both respond coherently to solar wind and magnetospheric driving. However, the response is independent of whether the storm response is associated with either a CME or CIR. Our analysis shows that during the initial phase, radiation belt loss is organized by the location of the magnetopause and the strength of Dst and ultralow frequency wave power. During the second phase, radiation belt enhancements are well organized by the amplitude of ultralow frequency waves, the auroral electroject index, and solar wind energy input. Overall, our results demonstrate that storm time dynamics of the RBC is repeatable and well characterized by solar wind and geomagnetic driving, albeit with different dependencies during the two phases of a storm.

中文翻译：

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理解和量化地磁暴期间外辐射带中相对论电子损失和加速的框架

我们对全球相对论电子动力学进行了详细分析，该动力学是通过在日冕物质抛射（CME）和同旋转相互作用区域（CIR）驱动的地磁风暴期间通过总辐射带含量（RBC）来测量的。最近的工作表明，地磁暴期间外辐射带的响应是一致且可重复的。在这里，我们基于这项工作来表明，辐射带动力学可以分为两个连续的阶段，这两个阶段具有不同的太阳风依赖性，并且如果单独分析，则表明辐射带的响应比整个风暴响应作为一个整体进行分析时更具预测性。 。就RBC而言，在我们分析的每场风暴中，以损耗为主的阶段之后是以加速为主的阶段。在每个阶段中对RBC的分析表明，它们都对太阳风和磁层驱动有一致的响应。但是，响应独立于风暴响应与CME还是CIR相关。我们的分析表明，在初始阶段，辐射带的损失是由磁顶的位置以及Dst和超低频波功率的强度来组织的。在第二阶段，通过超低频波的振幅，极光电注入指数和太阳风能输入，可以很好地组织辐射带的增强。总体而言，我们的结果表明，RBC的风暴时间动态是可重复的，并具有太阳风和地磁驱动的特征，尽管在风暴的两个阶段中它们具有不同的依赖性。