MHD turbulence and heating of the open field-line solar corona
MHD turbulence and heating of the open field-line solar corona
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DOI：
10.5194/npg-10-93-2003
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发表时间：
2003-01-01
影响因子：
2.2
通讯作者：
Oughton, S
中科院分区：
文献类型：
--
作者：
Matthaeus, WH;Mullan, DJ;Oughton, S
本文讨论的可能性，太阳日冕的加热在开放的场线区域发出的冕洞是由于一个非线性级联，驱动低频或准静态磁流体动力学波动。来自日冕不均匀性的反射在维持级联中起着重要的作用。物理和观测的限制进行了讨论。将级联能量转化为热量的动力学过程必须发生在湍流小尺度重联的区域，并且在某些方面可能类似于极光中观察到的强电子束引起的离子加热。
This paper discusses the possibility that heating of the solar corona in open field-line regions emanating from coronal holes is due to a nonlinear cascade, driven by low-frequency or quasi-static magnetohydrodynamic fluctuations. Reflection from coronal inhomogeneities plays an important role in sustaining the cascade. Physical and observational constraints are discussed. Kinetic processes that convert cascaded energy into heat must occur in regions of turbulent small-scale reconnection, and may be similar in some respects to ion heating due to intense electron beams observed in the aurora.