Angular momentum loss rates in Be stars determined by the viscous decretion disc model
Fil: Ghoreyshi, Maziar. University of Western Ontario. Department of Physics and Astronomy. Ontario, Canada.
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| Lenguaje: | Inglés |
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Oxford University Press
2023
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| Acceso en línea: | https://arxiv.org/abs/2210.14885 http://rid.unrn.edu.ar/handle/20.500.12049/10223 |
| Aporte de: |
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I65-R171-20.500.12049-10223 |
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dspace |
| institution |
Universidad Nacional de Río Negro |
| institution_str |
I-65 |
| repository_str |
R-171 |
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Repositorio Institucional Digital de la Universidad Nacional de Río Negro (UNRN) |
| language |
Inglés |
| orig_language_str_mv |
en |
| topic |
Astronomía stars: emission-line, Be stars: individual: ω CMa stars: massive stars: mass-loss stars: rotation Astronomía |
| spellingShingle |
Astronomía stars: emission-line, Be stars: individual: ω CMa stars: massive stars: mass-loss stars: rotation Astronomía Ghoreyshi, Maziar Jones, Carol E. Granada, Anahi Angular momentum loss rates in Be stars determined by the viscous decretion disc model |
| topic_facet |
Astronomía stars: emission-line, Be stars: individual: ω CMa stars: massive stars: mass-loss stars: rotation Astronomía |
| description |
Fil: Ghoreyshi, Maziar. University of Western Ontario. Department of Physics and Astronomy. Ontario, Canada. |
| author |
Ghoreyshi, Maziar Jones, Carol E. Granada, Anahi |
| author_facet |
Ghoreyshi, Maziar Jones, Carol E. Granada, Anahi |
| author_sort |
Ghoreyshi, Maziar |
| title |
Angular momentum loss rates in Be stars determined by the viscous decretion disc model |
| title_short |
Angular momentum loss rates in Be stars determined by the viscous decretion disc model |
| title_full |
Angular momentum loss rates in Be stars determined by the viscous decretion disc model |
| title_fullStr |
Angular momentum loss rates in Be stars determined by the viscous decretion disc model |
| title_full_unstemmed |
Angular momentum loss rates in Be stars determined by the viscous decretion disc model |
| title_sort |
angular momentum loss rates in be stars determined by the viscous decretion disc model |
| publisher |
Oxford University Press |
| publishDate |
2023 |
| url |
https://arxiv.org/abs/2210.14885 http://rid.unrn.edu.ar/handle/20.500.12049/10223 |
| work_keys_str_mv |
AT ghoreyshimaziar angularmomentumlossratesinbestarsdeterminedbytheviscousdecretiondiscmodel AT jonescarole angularmomentumlossratesinbestarsdeterminedbytheviscousdecretiondiscmodel AT granadaanahi angularmomentumlossratesinbestarsdeterminedbytheviscousdecretiondiscmodel |
| _version_ |
1767361990745915392 |
| spelling |
I65-R171-20.500.12049-102232023-05-24T13:24:18Z application/pdf info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/4.0/ 2023-01 Fil: Ghoreyshi, Maziar. University of Western Ontario. Department of Physics and Astronomy. Ontario, Canada. Fil: Jones, Carol E. University of Western Ontario. Department of Physics and Astronomy. Ontario, Canada. Fil: Granada, Anahi. Universidad Nacional de Rio Negro. Centro Interdisciplinario de Telecomunicaciones, Electrónica, Computación y Ciencia Aplicada. Rio Negro, Argentina. Fil: Granada, Anahi. Consejo Nacional de Investigaciones Científicas y Técnicas. Buenos Aires, Argentina. Angular momentum loss rates in Be stars determined by the viscous decretion disc model Ghoreyshi, Maziar Jones, Carol E. Granada, Anahi Astronomía stars: emission-line, Be stars: individual: ω CMa stars: massive stars: mass-loss stars: rotation Astronomía Circumstellar discs around Be stars are formed by the material ejected by the central star. This process removes excess angular momentum from the star as viscosity facilitates the mass and angular momentum transfer within the disc and its growth. The angular momentum loss rates (AMLR) of Be stars is a subject of debate in the literature. Through the modelling of the disc formation and dissipation phases observed from Be stars, their average AMLR can be determined and this is the goal of this work. We use the viscous decretion disc (VDD) model to provide a range of the average AMLR for Be stars and compare these rates with predicted values from the literature. We explore the reasons for discrepancies between the predicted values of average AMLR, using the VDD and Geneva stellar evolution models that were previously reported in literature and find that the largest differences occur when Be stars are rotating below their critical speeds. We show that the time over which the mass reservoir builds up is inversely proportional to the average AMLR. Also, we determine a revised value of the average AMLR for the Galactic Be star ω CMa of 4.7×1036gcm2s−2, which is in better agreement with the values expected for a typical B2-type star. Finally, the effect of disc truncation due to the presence of a companion star is investigated and we find that this has a minimal effect on the average AMLR. true Los discos circumestelares alrededor de las estrellas Be se forman por el material expulsado por la estrella central. Este proceso elimina el exceso de momento angular de la estrella, ya que la viscosidad facilita la transferencia de masa y momento angular dentro del disco y su crecimiento. Las tasas de pérdida de momento angular (AMLR) de las estrellas Be son objeto de debate en la literatura. A través de la modelización de las fases de formación y disipación del disco observadas en estrellas Be, se puede determinar su AMLR media y este es el objetivo de este trabajo. Utilizamos el modelo de disco de decrecimiento viscoso (VDD) para proporcionar un rango de la AMLR media de las estrellas Be y comparamos estas tasas con los valores predichos en la literatura. Exploramos las razones de las discrepancias entre los valores predichos de AMLR media, utilizando el modelo VDD y los modelos de evolución estelar de Ginebra de los que se había informado previamente en la literatura, y descubrimos que las mayores diferencias se producen cuando las estrellas Be están rotando por debajo de sus velocidades críticas. Demostramos que el tiempo durante el cual se acumula el depósito de masa es inversamente proporcional a la AMLR media. Además, determinamos un valor revisado de la AMLR media para la estrella galáctica Be ω CMa de 4,7×1036gcm2s-2, que concuerda mejor con los valores esperados para una estrella típica de tipo B2. Por último, se investiga el efecto del truncamiento del disco debido a la presencia de una estrella compañera y se observa que tiene un efecto mínimo sobre la AMLR media. M. R. Ghoreyshi, C. E. Jones, A. Granada (2023) Angular Momentum Loss Rates in Be Stars Determined by the Viscous Decretion Disc Model. Monthly Notices of the Royal Astronomical Society 0035-8711 https://arxiv.org/abs/2210.14885 http://rid.unrn.edu.ar/handle/20.500.12049/10223 en https://academic.oup.com/mnras Monthly Notices of the Royal Astronomical Society Oxford University Press |