MAGNETIC RECONNECTION IN CORONA AND LOOP PROMINENCE PHENOMENON
MAGNETIC RECONNECTION IN CORONA AND LOOP PROMINENCE PHENOMENON
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DOI：
10.1007/bf00206193
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发表时间：
1976-01-01
期刊：
影响因子：
2.8
通讯作者：
PNEUMAN, GW
中科院分区：
文献类型：
--
作者：
KOPP, RA;PNEUMAN, GW
许多种类的瞬变太阳现象，如耀斑，耀斑喷雾，和爆发的日冕，造成重大的破坏，在磁几何的覆盖日冕。通常情况下，天空实验室的结果表明，日冕中预先存在的闭合磁环被破坏的力量撕开。我们在这里研究一些理论上的后果，预计在扩展的松弛阶段，必须遵循这样的事件。这个阶段的特点是向外扩张的磁力线逐渐重新连接。特别是，增强的日冕膨胀发生在开放的场线之前，他们重新连接似乎足以提供大的向下的质量通量观察到的哈圈日珥系统，形成后瞬态松弛。此外，这种增强的流动可能会在这些事件之后在太阳风中产生非重现的高速流。松弛阶段的代表性领域的几何形状和由此产生的流配置的计算进行了说明。
Many classes of transient solar phenomena, such as flares, flare sprays, and eruptive prominences, cause major disruptions in the magnetic geometry of the overlying corona. Typically, the results from Skylab indicate that pre-existing closed magnetic loops in the corona are torn open by the force of the disruption. We examine here some of the theoretical consequences to be expected during the extended relaxation phase which must follow such events. This phase is characterized by a gradual reconnection of the outward-distended field lines. In particular, the enhanced coronal expansion which occurs on open field lines just before they reconnect appears adequate to supply the large downward mass fluxes observed in Ha loop prominence systems that form during the post-transient relaxation. In addition, this enhanced flow may produce nonrecurrent high speed streams in the solar wind after such events. Calculations of the relaxation phase for representative field geometries and the resulting flow configurations are described.