ABSTRACT We present a radiative magneto-hydrodynamic simulation set-up using the pencil code to study the generation, propagation and dissipation of Alfvén waves in the solar atmosphere which includes a convective layer, photosphere below and chromosphere, transition region and the corona above. We prepare a set-up of steady-state solar convection where the imposed external magnetic field also has reached the final value gradually starting from a very small value. From that state, we start several simulations by varying the magnetic Prandtl number and the forcing strengths. We find the propagation characteristics of waves excited in this simulation run depend strongly on the magnetic Prandtl number and the wave number of the forcing. For magnetic Prandtl number of unity, we obtain localised heating in the corona due to shock dissipation.

中文翻译：

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在“真实”的太阳大气环境中测试阿尔文波的传播

摘要 我们提出了一种使用铅笔代码的辐射磁流体动力学模拟装置，以研究太阳大气中阿尔文波的产生、传播和消散，其中包括对流层、下方的光球层和色球层、过渡区和上方的日冕。我们准备了一个稳态太阳对流的设置，其中施加的外部磁场也从一个非常小的值开始逐渐达到最终值。从那个状态开始，我们通过改变磁普朗特数和强迫强度来开始几次模拟。我们发现在此模拟运行中激发的波的传播特性强烈依赖于磁普朗特数和强迫波数。对于磁普朗特数的统一，我们在电晕中由于震动耗散而获得局部加热。