Ω-slow Solutions and Be Star Disks

As the disk formation mechanism(s) in Be stars is(are) as yet unknown, we investigate the role of rapidly rotating radiation-driven winds in this process. We implemented the effects of high stellar rotation on m-CAK models accounting for the shape of the star, the oblate finite disk correction facto...

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Detalles Bibliográficos
Autores principales:	Araya, I., Jones, C.E., Curé, M., Silaj, J., Cidale, Lydia Sonia, Granada, Anahí, Jiménez, A.
Formato:	Articulo
Lenguaje:	Inglés
Publicado:	2017
Materias:	Ciencias Astronómicas circumstellar matter hydrodynamics line: formation line: profiles stars: emissionline, Be
Acceso en línea:	http://sedici.unlp.edu.ar/handle/10915/87677
Aporte de:	SEDICI (UNLP) de Universidad Nacional de La Plata

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