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New mass-loss rates of B supergiants from global wind models
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SYSNO ASEP 0548202 Druh ASEP J - Článek v odborném periodiku Zařazení RIV J - Článek v odborném periodiku Poddruh J Článek ve WOS Název New mass-loss rates of B supergiants from global wind models Tvůrce(i) Krtička, J. (CZ)
Kubát, Jiří (ASU-R) RID, ORCID
Krtičková, I. (CZ)Číslo článku A28 Zdroj.dok. Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
Roč. 647, March (2021)Poč.str. 13 s. Forma vydání Online - E Jazyk dok. eng - angličtina Země vyd. FR - Francie Klíč. slova stars ; winds ; outflows Vědní obor RIV BN - Astronomie a nebeská mechanika, astrofyzika Obor OECD Astronomy (including astrophysics,space science) CEP Ga18-05665S GA ČR - Grantová agentura ČR Způsob publikování Open access s časovým embargem (01.04.2022) Institucionální podpora ASU-R - RVO:67985815 UT WOS 000626173100001 EID SCOPUS 85102031045 DOI 10.1051/0004-6361/202039900 Anotace Massive stars lose a significant fraction of mass during their evolution. However, the corresponding mass-loss rates are rather uncertain, especially for evolved stars. To improve this, we calculated global line-driven wind models for Galactic B supergiants. Our models predict radial wind structure and particularly the mass-loss rates and terminal velocities directly from basic stellar parameters. The hydrodynamic structure of the flow is consistently determined from the photosphere in nearly hydrostatic equilibrium to supersonically expanding wind. The radiative force is derived from the solution of the radiative transfer equation in the comoving frame. We provide a simple formula that predicts theoretical mass-loss rates as a function of stellar luminosity and effective temperature. The mass-loss rate of B supergiants slightly decreases with temperature down to about 22.5 kK, where the region of recombination of FeIV to FeIII starts to appear. In this region, which is about 5 kK wide, the mass-loss rate gradually increases by a factor of about 6. The increase of the mass-loss rate is associated with a gradual decrease of terminal velocities by a factor of about 2. We compared the predicted wind parameters with observations. Pracoviště Astronomický ústav Kontakt Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Rok sběru 2022 Elektronická adresa https://doi.org/10.1051/0004-6361/202039900
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