Direct Observational Evidence of Solar Wind Density Controlling the Evolution of the Ring Current During the 2024 October Major Storm

IF 2.4 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
Ming-Xian Zhao, Gui-Ming Le
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Abstract

We investigated the interplanetary source of the October 2024 major storm and determined that it was triggered by a sheath region and a magnetic cloud (MC), with the sheath region playing a decisive role. The MC has a larger and longer duration of southward interplanetary magnetic field (IMF) and solar wind electric field compared to the sheath, and the largest southward IMF and solar wind electric field were observed within the MC. As expect, the solar wind density in the sheath region is much larger than that in the MC. The results of this study not only provide direct evidence that solar wind density controls the evolution of the ring current, but also demonstrate that the correlation coefficients between the largest southward IMF and geomagnetic storm intensity, as well as between the largest solar wind electric field and geomagnetic storm intensity, lack physical meaning. The contribution of the sheath region to the intensity of the major storm, as estimated by the empirical formula developed by Burton, McPherron, and Russell (1975) (hereafter referred to as the BMR equation), was found to be smaller than that of the MC. However, actual observations indicate the opposite. This discrepancy suggests that the BMR equation is not capable of accurately estimating the ring current variation. The injection term in the BMR equation is merely a linear function of the solar wind electric field, without considering the solar wind density. This indicates that if we overlook the influence of solar wind density on the evolution of the ring current, estimating the intensity of a geomagnetic storm based solely on the integral of the solar wind electric field during the main phase of the storm would yield incorrect results. The October 2024 major storm also provides direct evidence that solar wind velocity, density, and the southward component of the IMF are all important parameters in the evolution of the ring current.

2024年10月大风暴期间太阳风密度控制环流演变的直接观测证据
我们研究了2024年10月大风暴的行星际来源,并确定它是由鞘区和磁云(MC)触发的,其中鞘区起着决定性作用。MC区南向行星际磁场(IMF)和太阳风电场的持续时间比鞘区大,且在MC区内观测到最大的南向行星际磁场和太阳风电场。正如预期的那样,鞘区太阳风密度远大于MC区。本研究结果不仅为太阳风密度控制环电流演化提供了直接证据,但也证明了最大南向国际货币基金组织与地磁风暴强度的相关系数,以及最大太阳风电场与地磁风暴强度的相关系数缺乏物理意义。根据Burton, mcphron, and Russell(1975)开发的经验公式(以下简称BMR方程),鞘区对大风暴强度的贡献小于MC。然而,实际观测结果显示相反。这种差异表明,BMR方程不能准确地估计环电流的变化。BMR方程中的注入项仅仅是太阳风电场的线性函数,没有考虑太阳风密度。这表明,如果忽略太阳风密度对环电流演变的影响,仅根据风暴主阶段太阳风电场的积分来估计地磁风暴的强度将会得到不正确的结果。2024年10月的大风暴也提供了直接证据,证明太阳风的速度、密度和IMF的南向分量都是环流演变的重要参数。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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来源期刊
Solar Physics
Solar Physics 地学天文-天文与天体物理
CiteScore
5.10
自引率
17.90%
发文量
146
审稿时长
1 months
期刊介绍: Solar Physics was founded in 1967 and is the principal journal for the publication of the results of fundamental research on the Sun. The journal treats all aspects of solar physics, ranging from the internal structure of the Sun and its evolution to the outer corona and solar wind in interplanetary space. Papers on solar-terrestrial physics and on stellar research are also published when their results have a direct bearing on our understanding of the Sun.
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