论文标题
恒星冠状和从太阳到M矮人的非线性alfvén波模型
Nonlinear Alfvén Wave Model of Stellar Coronae and Winds from the Sun to M dwarfs
论文作者
论文摘要
矮人的大气和风将被高度磁化。 Alfvén波的非线性传播在加热恒星气氛和驱动恒星风中都可以发挥关键作用。沿着这种Alfvén波的场景，我们进行了一维压缩磁性水力动力学（MHD）模拟，以了解从M矮人的光谱，染色体，染色体到电晕到电晕和跨界空间的非线性传播。基于模拟结果，我们开发了描述太阳和M矮人的冠状温度，恒星风速和风质量损失率的半经验方法。我们发现，M矮人的Coronae往往比太阳能电晕凉爽，并且与太阳风相比，M Dwarfs的恒星风将以更快的速度和更小的质量损失率来表征。
M dwarf's atmosphere and wind is expected to be highly magnetized. The nonlinear propagation of Alfvén wave could play a key role in both heating the stellar atmosphere and driving the stellar wind. Along this Alfvén wave scenario, we carried out the one-dimensional compressive magnetohydrodynamic (MHD) simulation about the nonlinear propagation of Alfvén wave from the M dwarf's photosphere, chromosphere to the corona and interplanetary space. Based on the simulation results, we develop the semi-empirical method describing the solar and M dwarf's coronal temperature, stellar wind velocity, and wind's mass loss rate. We find that M dwarfs' coronae tend to be cooler than solar corona, and that M dwarfs' stellar winds would be characterized with faster velocity and much smaller mass loss rate compared to those of the solar wind.
