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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Autores principales: | , , , , , , |
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Formato: | Articulo |
Lenguaje: | Inglés |
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2017
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Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/87677 |
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I19-R120-10915-87677 |
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dspace |
institution |
Universidad Nacional de La Plata |
institution_str |
I-19 |
repository_str |
R-120 |
collection |
SEDICI (UNLP) |
language |
Inglés |
topic |
Ciencias Astronómicas circumstellar matter hydrodynamics line: formation line: profiles stars: emissionline, Be |
spellingShingle |
Ciencias Astronómicas circumstellar matter hydrodynamics line: formation line: profiles stars: emissionline, Be Araya, I. Jones, C.E. Curé, M. Silaj, J. Cidale, Lydia Sonia Granada, Anahí Jiménez, A. Ω-slow Solutions and Be Star Disks |
topic_facet |
Ciencias Astronómicas circumstellar matter hydrodynamics line: formation line: profiles stars: emissionline, Be |
description |
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 factor, and gravity darkening. For a fast rotating star, we obtain a two-component wind model, i.e., a fast, thin wind in the polar latitudes and an Ω-slow, dense wind in the equatorial regions. We use the equatorial mass densities to explore Hα emission profiles for the following scenarios: (1) a spherically symmetric star, (2) an oblate star with constant temperature, and (3) an oblate star with gravity darkening. One result of this work is that we have developed a novel method for solving the gravity-darkened, oblate m-CAK equation of motion. Furthermore, from our modeling we find that (a) the oblate finite disk correction factor, for the scenario considering the gravity darkening, can vary by at least a factor of two between the equatorial and polar directions, influencing the velocity profile and mass-loss rate accordingly, (b) the Hα profiles predicted by our model are in agreement with those predicted by a standard power-law model for following values of the line-force parameters: , and , and (c) the contribution of the fast wind component to the Hα emission line profile is negligible; therefore, the line profiles arise mainly from the equatorial disks of Be stars. |
format |
Articulo Articulo |
author |
Araya, I. Jones, C.E. Curé, M. Silaj, J. Cidale, Lydia Sonia Granada, Anahí Jiménez, A. |
author_facet |
Araya, I. Jones, C.E. Curé, M. Silaj, J. Cidale, Lydia Sonia Granada, Anahí Jiménez, A. |
author_sort |
Araya, I. |
title |
Ω-slow Solutions and Be Star Disks |
title_short |
Ω-slow Solutions and Be Star Disks |
title_full |
Ω-slow Solutions and Be Star Disks |
title_fullStr |
Ω-slow Solutions and Be Star Disks |
title_full_unstemmed |
Ω-slow Solutions and Be Star Disks |
title_sort |
ω-slow solutions and be star disks |
publishDate |
2017 |
url |
http://sedici.unlp.edu.ar/handle/10915/87677 |
work_keys_str_mv |
AT arayai ōslowsolutionsandbestardisks AT jonesce ōslowsolutionsandbestardisks AT curem ōslowsolutionsandbestardisks AT silajj ōslowsolutionsandbestardisks AT cidalelydiasonia ōslowsolutionsandbestardisks AT granadaanahi ōslowsolutionsandbestardisks AT jimeneza ōslowsolutionsandbestardisks |
bdutipo_str |
Repositorios |
_version_ |
1764820489282256896 |