论文标题
在两米型耀斑上方的大规模电流板上撕裂模式的磁性重新连接的二维建模
Two-dimensional modeling of the tearing-mode-governed magnetic reconnection in the large-scale current sheet above the two-ribbon flare
论文作者
论文摘要
我们尝试使用2D模拟在重力分层的太阳大气中模拟磁性重新连接，其中Lundquist的$ s = 10^6 $。我们发现，撕裂模式的不稳定性导致重新连接电流（CS）内部的不均匀湍流，并调用重新连接的快速相位。快速重新连接带来了磁场的额外耗散，以明显的方式提高了重新连接率。 CS中的能量光谱显示了幂律模式和浆液的动力学控制相关光谱指数。我们注意到能量耗散发生在100-200 〜km的比例$ l_ {ko} $中，相关的CS厚度在1500至2500〜 km之间，它跟随Taylor scale $ l_t = l_t = l_ {ko} s^{1/6} $。终止冲击（TS）出现在耀斑环上方的湍流区域中，这是加热耀斑回路的重要原因。大量的磁能通过TS转化为动能和热能，累积加热速率大于动能转移的速率。另外，湍流在某种程度上通过TS扩增，其中幅度与TS的局部几何形状有关。
We attempt to model magnetic reconnection during the two-ribbon flare in the gravitationally stratified solar atmosphere with the Lundquist number of $S=10^6$ using 2D simulations. We found that the tearing mode instability leads to the inhomogeneous turbulence inside the reconnecting current sheet (CS) and invokes the fast phase of reconnection. Fast reconnection brings an extra dissipation of magnetic field which enhances the reconnection rate in an apparent way. The energy spectrum in the CS shows the power-law pattern and the dynamics of plasmoids governs the associated spectral index. We noticed that the energy dissipation occurs at a scale $l_{ko}$ of 100-200~km, and the associated CS thickness ranges from 1500 to 2500~km, which follows the Taylor scale $l_T=l_{ko} S^{1/6}$. The termination shock(TS) appears in the turbulent region above flare loops, which is an important contributor to heating flare loops. Substantial magnetic energy is converted into both kinetic and thermal energies via TS, and the cumulative heating rate is greater than the rate of the kinetic energy transfer. In addition, the turbulence is somehow amplified by TS, of which the amplitude is related to the local geometry of the TS.
