Photospheric magnetic vortex structures
Photospheric magnetic vortex structures
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DOI：
10.5194/angeo-29-883-2011
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发表时间：
2011-05
影响因子：
1.9
通讯作者：
S. Shelyag;V. Fedun;F. Keenan;R. Erdélyi;M. Mathioudakis
中科院分区：
文献类型：
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作者：
S. Shelyag;V. Fedun;F. Keenan;R. Erdélyi;M. Mathioudakis
抽象的。利用直接数值磁流体力学(MHD)模拟，我们证明了太阳光球中两种物理上不同类型的涡旋运动的证据。非磁性粒子中等离子体的斜压运动是太阳光球粒子区涡度的主要来源，然而，在强磁化的粒间带中有一个明显更有效的涡量产生机制。等离子体在晶间磁场密度下的这些漩涡运动可能导致不同类型的MHD波模的产生，例如扭结波、香肠波和扭转Alfven波。这些波可以从较低的太阳大气中输送相当数量的能量，并对日冕等离子体加热做出贡献。
Abstract. Using direct numerical magneto-hydrodynamic (MHD) simulations, we demonstrate the evidence of two physically different types of vortex motions in the solar photosphere. Baroclinic motions of plasma in non-magnetic granules are the primary source of vorticity in granular regions of the solar photosphere, however, there is a significantly more efficient mechanism of vorticity production in strongly magnetised intergranular lanes. These swirly motions of plasma in intergranular magnetic field concentrations could be responsible for the generation of different types of MHD wave modes, for example, kink, sausage and torsional Alfven waves. These waves could transport a relevant amount of energy from the lower solar atmosphere and contribute to coronal plasma heating.