MECHANISMS FOR MHD POYNTING FLUX GENERATION IN SIMULATIONS OF SOLAR PHOTOSPHERIC MAGNETOCONVECTION

被引：44
作者：
Shelyag, S. [1 ]
Mathioudakis, M. [1 ]
Keenan, F. P. [1 ]
机构：
[1] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland
来源：
ASTROPHYSICAL JOURNAL LETTERS | 2012年 / 753卷 / 01期
基金：
英国科学技术设施理事会;
关键词：
magnetohydrodynamics (MHD); plasmas; Sun: photosphere; Sun: surface magnetism; MAGNETIC-FIELD; DIAGNOSTICS; SUN;
D O I：
10.1088/2041-8205/753/1/L22
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We investigate the generation mechanisms of MHD Poynting flux in the magnetized solar photosphere. Using radiative MHD modeling of the solar photosphere with initial magnetic configurations that differ in their field strength and geometry, we show the presence of two different mechanisms for MHD Poynting flux generation in simulations of solar photospheric magnetoconvection. The weaker mechanism is connected to vertical transport of weak horizontal magnetic fields in the convectively stable layers of the upper photosphere, while the stronger is the production of Poynting flux in strongly magnetized intergranular lanes experiencing horizontal vortex motions. These mechanisms may be responsible for the energy transport from the solar convection zone to the higher layers of the solar atmosphere.
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页数：5
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