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Alfvén wave-driven wind from RGB and AGB stars

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Title: Alfvén wave-driven wind from RGB and AGB stars
Authors: Yasuda, Yuki Browse this author →KAKEN DB
Suzuki, Takeru K. Browse this author
Kozasa, Takashi Browse this author
Keywords: stars: late-type
stars: magnetic field
stars: mass-loss
stars: winds, outflows
Issue Date: 10-Jul-2019
Publisher: IOP Publishing
Journal Title: Astrophysical journal
Volume: 879
Issue: 2
Start Page: 77
Publisher DOI: 10.3847/1538-4357/ab23f7
Abstract: We develop a magnetohydrodynamical model of Alfven wave-driven wind in open magnetic flux tubes piercing the stellar surface of red giant branch (RGB) and asymptotic giant branch (AGB) stars, and investigate the physical properties of the winds. The model simulations are carried out along the evolutionary tracks of stars with initial mass in the range of 1.5-3.0 M-circle dot and initial metallicity Z(ini) = 0.02. Setting the surface magnetic field strength to 1 G, we find that the wind during the evolution of the star can be classified into the following four types: the first is wind with velocity higher than 80 km s(-1) in the RGB and early AGB (E-AGB) phases, the second is wind with outflow velocity less than 10 km s(-1) seen around the tip of the RGB or in the E-AGB phase, the third is the unstable wind in the E-AGB and thermally pulsing AGB (TP-AGB) phases, and the fourth is the stable massive and slow wind with mass-loss rate higher than 10 M-circle dot yr (-1) and outflow velocity lower than 20 km s(-1) in the TPAGB phase. The mass-loss rates in the first and second types of wind are two or three orders of magnitude lower than the values evaluated by an empirical formula. The presence of a massive and slow wind of the fourth type suggests the possibility that the massive outflow observed in TP-AGB stars could be attributed to Alfven wavedriven wind.
Type: article
Appears in Collections:理学院・理学研究院 (Graduate School of Science / Faculty of Science) > 雑誌発表論文等 (Peer-reviewed Journal Articles, etc)

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