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
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/37946

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network_name_str CONICET Digital (CONICET)
spelling 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
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https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
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