球壳中磁通量管的三维非线性演化：等熵情况
3-D non-linear evolution of a magnetic flux tube in a spherical shell: the isentropic case
摘要：
本文采用滞弹性球谐程序（ASH），对球形几何分层对流区中磁通量管的非线性动力学演化进行了三维MHD数值模拟。我们试图了解从太阳对流区底部到太阳表面作为活动区域的强环向场出现的机制。我们证实了在Carnival几何中得到的结果，即在到达对流区的顶部之前，没有扭曲的通量管分裂成两个相反的旋涡。此外，我们发现，扭曲管发生极向滑移不稳定性，由于不平衡的磁曲率力，使管的极向运动在非旋转和旋转的情况下。这种向极漂移被认为是更明显的管原本位于高纬度地区。最后，旋转被发现通过对流区的通量管的上升速度降低，特别是当该管被引入在低纬度。
英文摘要：
We present recent 3-D MHD numerical simulations of the non-linear dynamical evolution of magnetic flux tubes in an adiabatically stratified convection zone in spherical geometry, using the anelastic spherical harmonic (ASH) code. We seek to understand the mechanism of emergence of strong toroidal fields from the base of the solar convection zone to the solar surface as active regions. We confirm the results obtained in cartesian geometry that flux tubes that are not twisted split into two counter vortices before reaching the top of the convection zone. Moreover, we find that twisted tubes undergo the poleward-slip instability due to an unbalanced magnetic curvature force which gives the tube a poleward motion both in the non-rotating and in the rotating case. This poleward drift is found to be more pronounced on tubes originally located at high latitudes. Finally, rotation is found to decrease the rise velocity of the flux tubes through the convection zone, especially when the tube is introduced at low latitudes.
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