An anisotropic turbulent model for solar coronal heating
An anisotropic turbulent model for solar coronal heating
复制标题
太阳日冕加热的各向异性湍流模型
DOI：
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发表时间：
2007
期刊：
影响因子：
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通讯作者：
H. Politano
中科院分区：
文献类型：
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作者：
B. Bigot;S. Galtier;H. Politano
上下文我们提出了一个太阳日冕加热的自洽模型，其中我们包括沿着日冕结构的背景磁场的动力学效应，通过使用波MHD湍流的精确结果。目标。我们评估的加热速率和微湍流速度与观测比较，在安静的日冕，活动区，也冕洞。方法.日冕结构被认为是在一个动荡的状态维持缓慢的不稳定运动的磁足点。分别给出了大尺度动力学和未解决的小尺度动力学的描述。从后者，我们精确地计算（或数值冕洞）湍流粘性在前者中使用的自洽关闭系统，并推导出的热通量表达式。结果我们表明，加热速率和湍流速度与日冕观测相比毫不逊色。
Context. We present a self-consistent model of solar coronal heating in which we include the dynamical effect of the background magnetic field along a coronal structure by using exact results from wave MHD turbulence. Aims. We evaluate the heating rate and the microturbulent velocity for comparison with observations in the quiet corona, active regions and also coronal holes. Methods. The coronal structures are assumed to be in a turbulent state maintained by the slow erratic motion of the magnetic footpoints. A description of the large-scale and the unresolved small-scale dynamics are given separately. From the latter, we compute exactly (or numerically for coronal holes) turbulent viscosites used in the former to self-consistently close the system and derive the heating flux expression. Results. We show that the heating rate and the turbulent velocity compare favorably with coronal observations.