Physics of photospheric magnetic field

被引:0
|
作者
van Ballegooijen, AA [1 ]
Hasan, SS [1 ]
机构
[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
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中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The magnetic field on the quiet sun is continually swept into the intergranular lanes where it is amplified by interactions with the surrounding cool downflows. The resulting kilogauss flux tubes have typical sizes of about 100 km and magnetic field strengths of around 1500 G in the photosphere. A model of the magnetic field strength as function of depth is presented. It is shown that the Reynolds stress due to the downflows are sufficient to explain the observed kilogauss field strengths. We also present simulations of vorticity in intergranular lanes and the dynamics of flux tubes in response to such vortical motions. The simulations predict that flux tubes rotate with angular velocity similar to 5 x 10(-3) rad/s. If true, this would likely result in a significant flux of Alfven waves into the solar atmosphere that would contribute to the heating of the chromosphere and corona.
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页码:155 / 168
页数:14
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