Three‐dimensional magnetic flux rope structure formed by multiple sequential X‐line reconnection at the magnetopause
Three‐dimensional magnetic flux rope structure formed by multiple sequential X‐line reconnection at the magnetopause
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DOI：
10.1002/jgra.50281
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发表时间：
2013-04
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影响因子：
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通讯作者：
J. Zhong;Z. Pu;M. Dunlop;Y. Bogdanova;X. Wang;C. Xiao;R. Guo;H. Hasegawa;J. Raeder;X. Zhou;V. Angelopoulos;Q. Zong;S. Fu;L. Xie;M. Taylor;C. Shen;J. Berchem;Q. H. Zhang;M. Volwerk;J. Eastwood
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文献类型：
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作者：
J. Zhong;Z. Pu;M. Dunlop;Y. Bogdanova;X. Wang;C. Xiao;R. Guo;H. Hasegawa;J. Raeder;X. Zhou;V. Angelopoulos;Q. Zong;S. Fu;L. Xie;M. Taylor;C. Shen;J. Berchem;Q. H. Zhang;M. Volwerk;J. Eastwood
2007年6月14日，亚暴期间的四个事件时间历史和宏观尺度相互作用航天器观测到日侧磁层顶的通量转移事件（FTE），该事件先前已被证明是由二维背景下的多个连续X线重连（MSXR）产生的。本文报告了对MSXR事件的进一步研究，以显示基于额外测量的三维观点。通过对磁层顶两侧的多点测量，获得了穿越磁层边界的FTE通量绳的三维结构。通量绳的方向延伸部分大致位于磁层顶表面并平行于X线方向；而磁层分支的轴线基本上沿着局部的无扰动磁层场线。在磁通绳的中心区域，与传统观点不同，我们从电子分布中发现两种类型的磁场拓扑共存：连接磁层和磁鞘的开放磁场线和连接南北半球的封闭磁场线。因此，我们首次通过对磁场拓扑和磁通绳内等离子体分布的测定，确认了MSXR形成的三维重连磁通绳的特征特征。了解FTE通量绳的复杂几何结构将提高我们对太阳风-磁层相互作用的理解。
On 14 June 2007, four Time History of Events and Macroscale Interactions during Substorms spacecraft observed a flux transfer event (FTE) on the dayside magnetopause, which has been previously proved to be generated by multiple, sequential X‐line reconnection (MSXR) in a 2‐D context. This paper reports a further study of the MSXR event to show the 3‐D viewpoint based on additional measurements. The 3‐D structure of the FTE flux rope across the magnetospheric boundary is obtained on the basis of multipoint measurements taken on both sides of the magnetopause. The flux rope's azimuthally extended section is found to lie approximately on the magnetopause surface and parallel to the X‐line direction; while the axis of the magnetospheric branch is essentially along the local unperturbed magnetospheric field lines. In the central region of the flux rope, as distinct from the traditional viewpoint, we find from the electron distributions that two types of magnetic field topology coexist: opened magnetic field lines connecting the magnetosphere and the magnetosheath and closed field lines connecting the Southern and Northern hemispheres. We confirm, therefore, for the first time, the characteristic feature of the 3‐D reconnected magnetic flux rope, formed through MSXR, through a determination of the field topology and the plasma distributions within the flux rope. Knowledge of the complex geometry of FTE flux ropes will improve our understanding of solar wind‐magnetosphere interaction.