Numerical Simulations of the Flux Tube Tectonics Model for Coronal Heating
Numerical Simulations of the Flux Tube Tectonics Model for Coronal Heating
复制标题
日冕加热通量管构造模型的数值模拟
DOI：
10.1007/s11207-005-1713-2
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发表时间：
2005
期刊：
影响因子：
2.8
通讯作者：
E. Priest
中科院分区：
文献类型：
--
作者：
C. Mellor;C. Gerrard;K. Galsgaard;A. Hood;E. Priest
在本文中，我们介绍了三维MHD数值模拟的基础上提出的日冕加热的通量管构造方法的Priest，Heyvaerts，和标题（2002）。他们提出，个别的日冕环以许多不同的磁通量碎片连接到光球层，分界面存在于连接环到光球层的指状物之间和个别环之间。通量碎片的简单横向运动会导致电流沿着分界线集中，这可能会驱动重联，从而导致日冕加热。在这里，我们采取了一个简单的配置与四个通量补丁的顶部和底部的数值域和一个小的背景轴向场。然后，我们使用周期性边界条件将基座上的两个通量贴片移动到其他两个之间，使得当它们离开盒子时，它们在另一端重新进入盒子。这种简单的运动很快导致电流片沿着准分界线层沿着建立，随后发生磁扩散/重联。
In this paper we present results from 3D MHD numerical simulations based on the flux tube tectonics method of coronal heating proposed by Priest, Heyvaerts, and Title (2002). They suggested that individual coronal loops connect to the photosphere in many different magnetic flux fragments and that separatrix surfaces exist between the fingers connecting a loop to the photosphere and between individual loops. Simple lateral motions of the flux fragments could then cause currents to concentrate along the separatrices which may then drive reconnection contributing to coronal heating. Here we have taken a simple configuration with four flux patches on the top and bottom of the numerical domain and a small background axial field. Then we move two of the flux patches on the base between the other two using periodic boundary conditions such that when they leave the box they re-enter it at the other end. This simple motion soon causes current sheets to build up along the quasi-separatrix layers and subsequently magnetic diffusion/reconnection occurs.