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首页> 外文会议>Hinode Science Meeting >Two-Fluid Simulations of Chromospheric Heating by Alfvén Wave Pulses and Slow Magnetosonic Wave Pulses
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Two-Fluid Simulations of Chromospheric Heating by Alfvén Wave Pulses and Slow Magnetosonic Wave Pulses

机译：Alfvén波脉冲和慢磁音波脉冲的两种流体模拟

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摘要

We study a chromospheric heating process, via spontaneous excitation of Alfvén wave pulses and slow magnetosonic wave pulses. We use a two fluid (ion-neutral) numerical code to model the three-dimensional dynamics of protons and neutral-hydrogen particles, which couple through proton/neutral-hydrogen collisions. We model the convective neutral-hydrogen flows at the photospheric boundary, in an initially uniform vertical and oblique magnetic field. It was found that the down-flow regions, associated with convective motions, accumulate vertical magnetic fields, from where vertically propagating Alfvén and sound wave pulses are spontaneously generated. While in the oblique magnetic field, slow magnetosonic wave pulses are excited. Alfvén waves propagating in an initially vertical magnetic field with B_0 = 10~(-2) T strongly heat protons in the upper chromosphere, to temperatures of ≈ 3×10~5 K, while neutral-hydrogen is only weakly heated to ≈ 1.5 ×10~4 K. It was found that neutral-hydrogen is heated by dissipation of sound wave pulses, while the protons are collisionally heated by Alfvén wave pulses. We conclude that the energy flux transferred by the Alfvén wave pulses is sufficient to heat coronal regions to their observed temperatures.
机译：我们研究了色球加热过程中，通过阿尔芬波脉冲和慢磁声波脉冲的自发激发。我们使用两个流体（离子中性）数值代码质子和中性氢粒子的三维动力学，通过质子/中性氢碰撞，其耦合建模。我们在光球边界，对流中性氢流建模在初始均匀的垂直和倾斜磁场。已经发现，向下流动区域，与对流运动相关联，积累垂直磁场，从那里垂直传播阿尔芬和声波脉冲被自发产生的。而在倾斜磁场，慢磁声波脉冲被激发。阿尔芬波与初始垂直磁场传播B_0 = 10〜（-2）笔强烈加热在上色球质子，到≈3×10 -5 K，而中性氢仅微弱加热至≈1.5×温度10〜4 K.据发现，中性的氢被声波脉冲的耗散加热，而质子通过过碰撞阿尔芬波脉冲加热。我们的结论是由阿尔芬传送波脉冲的能量通量足以加热冠区域，以他们的观察到的温度。

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