Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars

Most radiation-driven winds of massive stars can be modelled with m-CAK theory, resulting in the so-called fast solution. However, the most rapidly rotating stars among them, especially when the rotational speed is higher than ∼75 per cent of the critical rotational speed, can adopt a different solu...

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Detalles Bibliográficos
Autores principales:	Araya, I., Curé, Michel, Doula, A. ud, Santillán, A., Cidale, Lydia Sonia
Formato:	Articulo
Lenguaje:	Inglés
Publicado:	2018
Materias:	Astronomía hydrodynamics stars: early-type stars: rotation stars: winds, outflows
Acceso en línea:	http://sedici.unlp.edu.ar/handle/10915/93912 https://academic.oup.com/mnras/article/477/1/755/4975263 https://ri.conicet.gov.ar/handle/11336/82696
Aporte de:	SEDICI (UNLP) de Universidad Nacional de La Plata

id	I19-R120-10915-93912
record_format	dspace
institution	Universidad Nacional de La Plata
institution_str	I-19
repository_str	R-120
collection	SEDICI (UNLP)
language	Inglés
topic	Astronomía hydrodynamics stars: early-type stars: rotation stars: winds, outflows
spellingShingle	Astronomía hydrodynamics stars: early-type stars: rotation stars: winds, outflows Araya, I. Curé, Michel Doula, A. ud Santillán, A. Cidale, Lydia Sonia Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
topic_facet	Astronomía hydrodynamics stars: early-type stars: rotation stars: winds, outflows
description	Most radiation-driven winds of massive stars can be modelled with m-CAK theory, resulting in the so-called fast solution. However, the most rapidly rotating stars among them, especially when the rotational speed is higher than ∼75 per cent of the critical rotational speed, can adopt a different solution, the so-called Ω-slow solution, characterized by a dense and slow wind. Here, we study the transition region of the solutions where the fast solution changes to the Ω-slow solution. Using both time-steady and time-dependent numerical codes, we study this transition region for various equatorial models of B-type stars. In all cases, in a certain range of rotational speeds we find a region where the fast and the Ω-slow solution can coexist. We find that the type of solution obtained in this co-existence region depends stongly on the initial conditions of our models. We also test the stability of the solutions within the co-existence region by performing base-density perturbations in the wind. We find that under certain conditions, the fast solution can switch to the Ω-slow solution, or vice versa. Such solution-switching may be a possible contributor of material injected into the circumstellar environment of Be stars, without requiring rotational speeds near critical values.
format	Articulo Articulo
author	Araya, I. Curé, Michel Doula, A. ud Santillán, A. Cidale, Lydia Sonia
author_facet	Araya, I. Curé, Michel Doula, A. ud Santillán, A. Cidale, Lydia Sonia
author_sort	Araya, I.
title	Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
title_short	Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
title_full	Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
title_fullStr	Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
title_full_unstemmed	Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars
title_sort	co-existence and switching between fast and ω-slow wind solutions in rapidly rotating massive stars
publishDate	2018
url	http://sedici.unlp.edu.ar/handle/10915/93912 https://academic.oup.com/mnras/article/477/1/755/4975263 https://ri.conicet.gov.ar/handle/11336/82696
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bdutipo_str	Repositorios
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Co-existence and switching between fast and Ω-slow wind solutions in rapidly rotating massive stars

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