Three-dimensional modeling of coronal magnetic fields

被引：0
|
作者：
van Ballegooijen, AA [1 ]
机构：
[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
来源：
ADVANCED SOLAR POLARIMETRY: THEORY, OBSERVATION, AND INSTRUMENTA TION | 2001年 / 236卷
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D O I：
暂无
中图分类号：
V [航空、航天];
学科分类号：
08 ; 0825 ;
摘要：
The coronal magnetic field evolves in response to motions of the photospheric footpoints of coronal field lines. These motions include the effects of the solar differential rotation, meridional flows, and supergranular diffusion. Simulations have shown that these flows can lead to the formation of highly sheared or helical magnetic fields in the corona. Here we review recent modeling of such non-potential magnetic structures, and we discuss the relevance of these models to observations of filaments and prominences.
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页码：235 / 243
页数：9
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