Rappazzo A F, Velli M
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain.
Phys Rev E Stat Nonlin Soft Matter Phys. 2011 Jun;83(6 Pt 2):065401. doi: 10.1103/PhysRevE.83.065401. Epub 2011 Jun 10.
The Parker model for coronal heating is investigated through a high resolution simulation. An inertial range is resolved where fluctuating magnetic energy EMk[Please see symbol]) [Please see symbol] kPlease see symbol exceeds kinetic energy EK(k[Please see symbol])[Please see symbol]kPlease see symbol. Increments scale as δbℓ ~/= ℓ(-0.85) and δuℓ ~/= ℓ(+0.2) with velocity increasing at small scales, indicating that magnetic reconnection plays a prime role in this turbulent system. We show that spectral energy transport is akin to standard magnetohydrodynamic (MHD) turbulence even for a system of reconnecting current sheets sustained by the boundary. In this new MHD turbulent cascade, kinetic energy flows are negligible while cross-field flows are enhanced, and through a series of "reflections" between the two fields, cascade more than half of the total spectral energy flow.
通过高分辨率模拟研究了帕克日冕加热模型。解析出一个惯性范围，其中波动磁能(E_{Mk})（请见符号）(\propto k^{-2.7})超过动能(E_{K}(k))（请见符号）(\propto k^{-0.6})。增量尺度为(\delta b_{\ell}\sim\ell^{-0.85})和(\delta u_{\ell}\sim\ell^{+0.2})，速度在小尺度上增加，这表明磁重联在这个湍流系统中起主要作用。我们表明，即使对于由边界维持的重接电流片系统，谱能量传输也类似于标准磁流体动力学（MHD）湍流。在这个新的MHD湍流级联中，动能流可以忽略不计，而跨场流增强，并且通过两个场之间的一系列“反射”，级联了超过一半的总谱能量流。
