Geometry of interplanetary magnetic clouds
Geometry of interplanetary magnetic clouds
复制标题
行星际磁云的几何形状
DOI：
10.1029/95gl00013
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发表时间：
1995
影响因子：
5.2
通讯作者：
S. Zalesak
中科院分区：
文献类型：
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作者：
P. Cargill;James Chen;D. Spicer;S. Zalesak
本文对太阳风等离子体加速过程中磁通绳的畸变进行了二维磁流体力学模拟。磁通绳磁场具有平行于太阳风场的轴向分量和位于模拟平面的方位角分量。当通量绳穿过太阳风等离子体时，在其后缘形成漩涡，并与内部强烈耦合。如果通量绳的方位角场较弱，在经过几次阿尔芬凌日之后，它就会变形成细长的香蕉状。强的方位场分量倾向于抑制这种畸变。如果用通量绳来模拟磁云，则建议在1au处的磁云的形状是由其在内太阳风中的畸变决定的。超过1天文单位的扭曲时间尺度估计为许多天。估计用大于1的有效阻力系数来模拟磁链的传播是合适的。
Two dimensional magnetohydrodynamic simulations are presented of the distortion of a magnetic flux rope that is being accelerated through ambient solar wind plasma. The flux rope magnetic field has an axial component parallel to the solar wind field and an azimuthal component, which lies in the simulation plane. As the flux rope moves through the solar wind plasma, vortices form on its trailing edge and couple strongly to its interior. If the flux rope azimuthal field is weak, it deforms into an elongated banana-like shape after a few Alfven transit times. A strong azimuthal field component tends to inhibit this distortion. If the flux rope is taken to model a magnetic cloud, it is suggested that the shape of the cloud at 1 AU is determined by its distortion in the inner solar wind. Distortion timescales beyond 1 AU are estimated as many days. It is estimated that effective drag coefficients somewhat greater than unity are appropriate for modelling flux rope propagation.
Y.Iwata 等人：Nucl.Instr.Methods。
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