Critical study of the distribution of rotational velocities of Be stars, I : deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity
- Autores
- Zorec, J.; Fremat, Y; Domiciano de Souza, A.; Royer, F.; Cidale, Lydia Sonia; Hubert, A.-M.; Semaan, T.; Martayan, C; Cochetti, Yanina Roxana; Arias, M. L.; Aidelman, Yael Judith; Stee, P.
- Año de publicación
- 2016
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. Among intermediate-mass and massive stars, Be stars are the fastest rotators in the main sequence (MS) and, as such, these stars are a cornerstone to validate models of structure and evolution of rotating stars. Several phenomena, however, induce under- or overestimations either of their apparent Vsini, or true velocity V.Aims. In the present contribution we aim at obtaining distributions of true rotational velocities corrected for systematic effects induced by the rapid rotation itself, macroturbulent velocities, and binarity.Methods. We study a set of 233 Be stars by assuming they have inclination angles distributed at random. We critically discuss the methods of Cranmer and Lucy-Richardson, which enable us to transform a distribution of projected velocities into another distribution of true rotational velocities, where the gravitational darkening effect on the Vsini parameter is considered in different ways. We conclude that iterative algorithm by Lucy-Richardson responds at best to the purposes of the present work, but it requires a thorough determination of the stellar fundamental parameters.Results. We conclude that once the mode of ratios of the true velocities of Be stars attains the value V/Vc ≃ 0.77 in the main-sequence (MS) evolutionary phase, it remains unchanged up to the end of the MS lifespan. The statistical corrections found on the distribution of ratios V/Vc for overestimations of Vsini, due to macroturbulent motions and binarity, produce a shift of this distribution toward lower values of V/Vc when Be stars in all MS evolutionary stages are considered together. The mode of the final distribution obtained is at V/Vc ≃ 0.65. This distribution has a nearly symmetric distribution and shows that the Be phenomenon is characterized by a wide range of true velocity ratios 0.3 ≲ V/Vc ≲ 0.95. It thus suggests that the probability that Be stars are critical rotators is extremely low.Conclusions. The corrections attempted in the present work represent an initial step to infer indications about the nature of the Be-star surface rotation that will be studied in the second paper of this series.
Fil: Zorec, J.. Institut d’Astrophysique de Paris; Francia
Fil: Fremat, Y. Institut d’Astrophysique de Paris; Francia
Fil: Domiciano de Souza, A.. Observatoire de la Côte d’Azur; Francia
Fil: Royer, F.. Université Paris Diderot - Paris 7; Francia
Fil: Cidale, Lydia Sonia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Hubert, A.-M.. Université Paris Diderot - Paris 7; Francia
Fil: Semaan, T.. University of Geneva; Suiza
Fil: Martayan, C. European Organization for Astronomical Research in the Southern Hemisphere; Chile
Fil: Cochetti, Yanina Roxana. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Arias, M. L.. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Aidelman, Yael Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Stee, P.. Observatoire de la Côte d’Azur; Francia - Materia
-
Emission Line
Be Stars
Rotation - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/37946
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oai:ri.conicet.gov.ar:11336/37946 |
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Critical study of the distribution of rotational velocities of Be stars, I : deconvolution methods, effects due to gravity darkening, macroturbulence, and binarityZorec, J.Fremat, YDomiciano de Souza, A.Royer, F.Cidale, Lydia SoniaHubert, A.-M.Semaan, T.Martayan, CCochetti, Yanina RoxanaArias, M. L.Aidelman, Yael JudithStee, P.Emission LineBe StarsRotationhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Among intermediate-mass and massive stars, Be stars are the fastest rotators in the main sequence (MS) and, as such, these stars are a cornerstone to validate models of structure and evolution of rotating stars. Several phenomena, however, induce under- or overestimations either of their apparent Vsini, or true velocity V.Aims. In the present contribution we aim at obtaining distributions of true rotational velocities corrected for systematic effects induced by the rapid rotation itself, macroturbulent velocities, and binarity.Methods. We study a set of 233 Be stars by assuming they have inclination angles distributed at random. We critically discuss the methods of Cranmer and Lucy-Richardson, which enable us to transform a distribution of projected velocities into another distribution of true rotational velocities, where the gravitational darkening effect on the Vsini parameter is considered in different ways. We conclude that iterative algorithm by Lucy-Richardson responds at best to the purposes of the present work, but it requires a thorough determination of the stellar fundamental parameters.Results. We conclude that once the mode of ratios of the true velocities of Be stars attains the value V/Vc ≃ 0.77 in the main-sequence (MS) evolutionary phase, it remains unchanged up to the end of the MS lifespan. The statistical corrections found on the distribution of ratios V/Vc for overestimations of Vsini, due to macroturbulent motions and binarity, produce a shift of this distribution toward lower values of V/Vc when Be stars in all MS evolutionary stages are considered together. The mode of the final distribution obtained is at V/Vc ≃ 0.65. This distribution has a nearly symmetric distribution and shows that the Be phenomenon is characterized by a wide range of true velocity ratios 0.3 ≲ V/Vc ≲ 0.95. It thus suggests that the probability that Be stars are critical rotators is extremely low.Conclusions. The corrections attempted in the present work represent an initial step to infer indications about the nature of the Be-star surface rotation that will be studied in the second paper of this series.Fil: Zorec, J.. Institut d’Astrophysique de Paris; FranciaFil: Fremat, Y. Institut d’Astrophysique de Paris; FranciaFil: Domiciano de Souza, A.. Observatoire de la Côte d’Azur; FranciaFil: Royer, F.. Université Paris Diderot - Paris 7; FranciaFil: Cidale, Lydia Sonia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Hubert, A.-M.. Université Paris Diderot - Paris 7; FranciaFil: Semaan, T.. University of Geneva; SuizaFil: Martayan, C. European Organization for Astronomical Research in the Southern Hemisphere; ChileFil: Cochetti, Yanina Roxana. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Arias, M. L.. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Aidelman, Yael Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Stee, P.. Observatoire de la Côte d’Azur; FranciaEDP Sciences2016-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/37946Zorec, J.; Fremat, Y; Domiciano de Souza, A.; Royer, F.; Cidale, Lydia Sonia; et al.; Critical study of the distribution of rotational velocities of Be stars, I : deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity; EDP Sciences; Astronomy and Astrophysics; 595; 595; 11-2016; A1320004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628760info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2016/11/aa28760-16/aa28760-16.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:19:14Zoai:ri.conicet.gov.ar:11336/37946instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-15 15:19:15.235CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Critical study of the distribution of rotational velocities of Be stars, I : deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity |
title |
Critical study of the distribution of rotational velocities of Be stars, I : deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity |
spellingShingle |
Critical study of the distribution of rotational velocities of Be stars, I : deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity Zorec, J. Emission Line Be Stars Rotation |
title_short |
Critical study of the distribution of rotational velocities of Be stars, I : deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity |
title_full |
Critical study of the distribution of rotational velocities of Be stars, I : deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity |
title_fullStr |
Critical study of the distribution of rotational velocities of Be stars, I : deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity |
title_full_unstemmed |
Critical study of the distribution of rotational velocities of Be stars, I : deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity |
title_sort |
Critical study of the distribution of rotational velocities of Be stars, I : deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity |
dc.creator.none.fl_str_mv |
Zorec, J. Fremat, Y Domiciano de Souza, A. Royer, F. Cidale, Lydia Sonia Hubert, A.-M. Semaan, T. Martayan, C Cochetti, Yanina Roxana Arias, M. L. Aidelman, Yael Judith Stee, P. |
author |
Zorec, J. |
author_facet |
Zorec, J. Fremat, Y Domiciano de Souza, A. Royer, F. Cidale, Lydia Sonia Hubert, A.-M. Semaan, T. Martayan, C Cochetti, Yanina Roxana Arias, M. L. Aidelman, Yael Judith Stee, P. |
author_role |
author |
author2 |
Fremat, Y Domiciano de Souza, A. Royer, F. Cidale, Lydia Sonia Hubert, A.-M. Semaan, T. Martayan, C Cochetti, Yanina Roxana Arias, M. L. Aidelman, Yael Judith Stee, P. |
author2_role |
author author author author author author author author author author author |
dc.subject.none.fl_str_mv |
Emission Line Be Stars Rotation |
topic |
Emission Line Be Stars Rotation |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Context. Among intermediate-mass and massive stars, Be stars are the fastest rotators in the main sequence (MS) and, as such, these stars are a cornerstone to validate models of structure and evolution of rotating stars. Several phenomena, however, induce under- or overestimations either of their apparent Vsini, or true velocity V.Aims. In the present contribution we aim at obtaining distributions of true rotational velocities corrected for systematic effects induced by the rapid rotation itself, macroturbulent velocities, and binarity.Methods. We study a set of 233 Be stars by assuming they have inclination angles distributed at random. We critically discuss the methods of Cranmer and Lucy-Richardson, which enable us to transform a distribution of projected velocities into another distribution of true rotational velocities, where the gravitational darkening effect on the Vsini parameter is considered in different ways. We conclude that iterative algorithm by Lucy-Richardson responds at best to the purposes of the present work, but it requires a thorough determination of the stellar fundamental parameters.Results. We conclude that once the mode of ratios of the true velocities of Be stars attains the value V/Vc ≃ 0.77 in the main-sequence (MS) evolutionary phase, it remains unchanged up to the end of the MS lifespan. The statistical corrections found on the distribution of ratios V/Vc for overestimations of Vsini, due to macroturbulent motions and binarity, produce a shift of this distribution toward lower values of V/Vc when Be stars in all MS evolutionary stages are considered together. The mode of the final distribution obtained is at V/Vc ≃ 0.65. This distribution has a nearly symmetric distribution and shows that the Be phenomenon is characterized by a wide range of true velocity ratios 0.3 ≲ V/Vc ≲ 0.95. It thus suggests that the probability that Be stars are critical rotators is extremely low.Conclusions. The corrections attempted in the present work represent an initial step to infer indications about the nature of the Be-star surface rotation that will be studied in the second paper of this series. Fil: Zorec, J.. Institut d’Astrophysique de Paris; Francia Fil: Fremat, Y. Institut d’Astrophysique de Paris; Francia Fil: Domiciano de Souza, A.. Observatoire de la Côte d’Azur; Francia Fil: Royer, F.. Université Paris Diderot - Paris 7; Francia Fil: Cidale, Lydia Sonia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Hubert, A.-M.. Université Paris Diderot - Paris 7; Francia Fil: Semaan, T.. University of Geneva; Suiza Fil: Martayan, C. European Organization for Astronomical Research in the Southern Hemisphere; Chile Fil: Cochetti, Yanina Roxana. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Arias, M. L.. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Aidelman, Yael Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Stee, P.. Observatoire de la Côte d’Azur; Francia |
description |
Context. Among intermediate-mass and massive stars, Be stars are the fastest rotators in the main sequence (MS) and, as such, these stars are a cornerstone to validate models of structure and evolution of rotating stars. Several phenomena, however, induce under- or overestimations either of their apparent Vsini, or true velocity V.Aims. In the present contribution we aim at obtaining distributions of true rotational velocities corrected for systematic effects induced by the rapid rotation itself, macroturbulent velocities, and binarity.Methods. We study a set of 233 Be stars by assuming they have inclination angles distributed at random. We critically discuss the methods of Cranmer and Lucy-Richardson, which enable us to transform a distribution of projected velocities into another distribution of true rotational velocities, where the gravitational darkening effect on the Vsini parameter is considered in different ways. We conclude that iterative algorithm by Lucy-Richardson responds at best to the purposes of the present work, but it requires a thorough determination of the stellar fundamental parameters.Results. We conclude that once the mode of ratios of the true velocities of Be stars attains the value V/Vc ≃ 0.77 in the main-sequence (MS) evolutionary phase, it remains unchanged up to the end of the MS lifespan. The statistical corrections found on the distribution of ratios V/Vc for overestimations of Vsini, due to macroturbulent motions and binarity, produce a shift of this distribution toward lower values of V/Vc when Be stars in all MS evolutionary stages are considered together. The mode of the final distribution obtained is at V/Vc ≃ 0.65. This distribution has a nearly symmetric distribution and shows that the Be phenomenon is characterized by a wide range of true velocity ratios 0.3 ≲ V/Vc ≲ 0.95. It thus suggests that the probability that Be stars are critical rotators is extremely low.Conclusions. The corrections attempted in the present work represent an initial step to infer indications about the nature of the Be-star surface rotation that will be studied in the second paper of this series. |
publishDate |
2016 |
dc.date.none.fl_str_mv |
2016-11 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
format |
article |
status_str |
publishedVersion |
dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/37946 Zorec, J.; Fremat, Y; Domiciano de Souza, A.; Royer, F.; Cidale, Lydia Sonia; et al.; Critical study of the distribution of rotational velocities of Be stars, I : deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity; EDP Sciences; Astronomy and Astrophysics; 595; 595; 11-2016; A132 0004-6361 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/37946 |
identifier_str_mv |
Zorec, J.; Fremat, Y; Domiciano de Souza, A.; Royer, F.; Cidale, Lydia Sonia; et al.; Critical study of the distribution of rotational velocities of Be stars, I : deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity; EDP Sciences; Astronomy and Astrophysics; 595; 595; 11-2016; A132 0004-6361 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628760 info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2016/11/aa28760-16/aa28760-16.html |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
EDP Sciences |
publisher.none.fl_str_mv |
EDP Sciences |
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reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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1846083341416136704 |
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13.22299 |