Nonlinear Alfven Wave Model of Stellar Coronae and Winds from the Sun to M Dwarfs

被引:5
作者
Sakaue, Takahito [1 ]
Shibata, Kazunari [1 ]
机构
[1] Kyoto Univ, Astron Observ, Kyoto, Japan
关键词
Stellar winds; Stellar coronae; Stellar chromospheres; M dwarf stars; Alfven waves; Magnetohydrodynamics; EARTH-LIKE EXOPLANETS; EJECTION CME ACTIVITY; MASS M-STARS; TERRESTRIAL EXOPLANETS; SOLAR-WIND; HABITABILITY; PLANETS; PROPAGATION; SIMULATIONS; IDEAL;
D O I
10.3847/2041-8213/abd3a9
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
An M dwarf's atmosphere and wind are expected to be highly magnetized. The nonlinear propagation of Alfven waves could play a key role in both heating the stellar atmosphere and driving the stellar wind. Using this Alfven wave scenario, we carried out a one-dimensional compressive magnetohydrodynamic simulation to examine the nonlinear propagation of Alfven waves from the M dwarf's photosphere, chromosphere to the corona, and interplanetary space. Based on the simulation results, we developed a 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 the solar corona, and that M dwarfs' stellar winds can be characterized as having a faster velocity and much smaller mass-loss rate compared to those of the solar wind.
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页数:7
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