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

  • Authors: Takahito Sakaue, and Kazunari Shibata

2021 The Astrophysical Journal Letters 906 L13.

  • Provider: AAS Journals

Caption: Figure 5.

General trends of stellar wind velocity (vwind), coronal temperature (Tco), and wind’s mass-loss rate (﹩\dot{M}﹩), with respect to the effective temperature (Teff) and Alfvén wave luminosity on the photosphere (LA,ph), which is predicted by our semi-empirical method. The open circles in this figure represent part of the samples in our parameter survey. The thick dashed line corresponds to the fiducial LA,ph as a function of Teff. The thick dashed–dotted line corresponds to the largest LA,ph obtained by assuming that the convective velocity reaches the sound speed on the photosphere. The thin dashed line represents LA,ph as a function of Teff, which results in vwind = vesc⋆.

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