论文标题
太阳风的完全可压缩的3D磁水动力模拟
Full compressible 3D magnetohydrodynamic simulation of solar wind
论文作者
论文摘要
确定太阳能电晕的加热机制和太阳风的驾驶机制是理解太阳能物理学的关键挑战。进行了完整的三维可压缩磁性水力动力学（MHD）模拟，以区分开放场区域上方的快速太阳风中的加热机理。我们的仿真描述了AlfvénicWaves的演变，其中包括从光球到Heliospheric距离$ s $ 27太阳RADII（$ r_ \ odot $）的可压缩效果。由于Alfvén波的耗散，同时再现了热的电晕和快速的太阳风。过渡区域和较低气氛的包括使我们能够通过执行完整的三维可压缩MHD模拟来首次得出太阳质量损失率。如先前的太阳风模型所建议，AlfVén湍流被确定为太阳风加速度区域（$ s> 1.3 r_ \ odot $）的主要加热机理。此外，冲击形成和相位混合也很重要，低于下过渡区域（$ s <1.03R_ \ odot $）。
Identifying the heating mechanisms of the solar corona and the driving mechanisms of solar wind are key challenges in understanding solar physics. A full three-dimensional compressible magnetohydrodynamic (MHD) simulation was conducted to distinguish between the heating mechanisms in the fast solar wind above the open field region. Our simulation describes the evolution of the Alfvénic waves, which includes the compressible effects from the photosphere to the heliospheric distance $s$ of 27 solar radii ($R_\odot$). The hot corona and fast solar wind were reproduced simultaneously due to the dissipation of the Alfvén waves. The inclusion of the transition region and lower atmosphere enabled us to derive the solar mass loss rate for the first time by performing a full three-dimensional compressible MHD simulation. The Alfvén turbulence was determined to be the dominant heating mechanism in the solar wind acceleration region ($s>1.3 R_\odot$), as suggested by previous solar wind models. In addition, shock formation and phase mixing are important below the lower transition region ($s<1.03R_\odot$) as well.
