Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion

Autores
Benvenuto, Omar Gustavo; Serenelli, A. M.; Althaus, Leandro Gabriel; Barba, Rodolfo Hector; Morrell, Nidia Irene
Año de publicación
2002
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present a method to calculate masses for components of both eclipsing and non-eclipsing binary systems as long as their apsidal motion rates are available. The method is based on the fact that the equation that gives the rate of apsidal motion is a supplementary equation that allows the computation of the masses of the components, if their radii and the internal structure constants can be obtained from theoretical models. For this reason the use of this equation makes the method presented here model dependent. We apply this method to calculate the mass of the components of the non-eclipsing massive binary system HD 93205 (O3 V + O8 V), which is suspected to be a very young system. To this end, we have computed a grid of evolutionary models covering the mass range of interest, and taking the mass of the primary (M1) as the only independent variable, we solve the equation of apsidal motion for M1 as a function of the age of the system. The mass of the primary that we find ranges from M1 = 60 ± 19 M⊙ for zero-age main-sequence models, which sets an upper limit for M1, down to M1 = 40 ± 9 M⊙ for an age of 2 Myr. Accordingly, the upper limit derived for the mass of the secondary (M2 = QM1) M2 = 25 M⊙ is in very good agreement with the masses derived for other O8 V stars occurring in eclipsing binaries.
Fil: Benvenuto, Omar Gustavo. 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
Fil: Serenelli, A. M.. Universidad Nacional de La Plata; Argentina
Fil: Althaus, Leandro Gabriel. 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
Fil: Barba, Rodolfo Hector. Universidad Nacional de La Plata; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Morrell, Nidia Irene. 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
Materia
BINARIES: ECLIPSING
STARS: EARLY-TYPE
STARS: EVOLUTION
STARS: FUNDAMENTAL PARAMETERS
STARS: INDIVIDUAL: HD 93205
STARS: INTERIORS
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:11336/36895
Acceder
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network_name_str CONICET Digital (CONICET)
spelling Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motionBenvenuto, Omar GustavoSerenelli, A. M.Althaus, Leandro GabrielBarba, Rodolfo HectorMorrell, Nidia IreneBINARIES: ECLIPSINGSTARS: EARLY-TYPESTARS: EVOLUTIONSTARS: FUNDAMENTAL PARAMETERSSTARS: INDIVIDUAL: HD 93205STARS: INTERIORShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present a method to calculate masses for components of both eclipsing and non-eclipsing binary systems as long as their apsidal motion rates are available. The method is based on the fact that the equation that gives the rate of apsidal motion is a supplementary equation that allows the computation of the masses of the components, if their radii and the internal structure constants can be obtained from theoretical models. For this reason the use of this equation makes the method presented here model dependent. We apply this method to calculate the mass of the components of the non-eclipsing massive binary system HD 93205 (O3 V + O8 V), which is suspected to be a very young system. To this end, we have computed a grid of evolutionary models covering the mass range of interest, and taking the mass of the primary (M1) as the only independent variable, we solve the equation of apsidal motion for M1 as a function of the age of the system. The mass of the primary that we find ranges from M1 = 60 ± 19 M⊙ for zero-age main-sequence models, which sets an upper limit for M1, down to M1 = 40 ± 9 M⊙ for an age of 2 Myr. Accordingly, the upper limit derived for the mass of the secondary (M2 = QM1) M2 = 25 M⊙ is in very good agreement with the masses derived for other O8 V stars occurring in eclipsing binaries.Fil: Benvenuto, Omar Gustavo. 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; ArgentinaFil: Serenelli, A. M.. Universidad Nacional de La Plata; ArgentinaFil: Althaus, Leandro Gabriel. 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; ArgentinaFil: Barba, Rodolfo Hector. Universidad Nacional de La Plata; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Morrell, Nidia Irene. 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; ArgentinaWiley Blackwell Publishing, Inc2002-02info: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/11336/36895Benvenuto, Omar Gustavo; Serenelli, A. M.; Althaus, Leandro Gabriel; Barba, Rodolfo Hector; Morrell, Nidia Irene; Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 330; 2; 2-2002; 435-4420035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://onlinelibrary.wiley.com/doi/10.1046/j.1365-8711.2002.05083.x/abstractinfo:eu-repo/semantics/altIdentifier/doi/10.1046/j.1365-8711.2002.05083.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/330/2/435/1083947info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:55:48Zoai:ri.conicet.gov.ar:11336/36895instacron: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:34982025-09-29 09:55:48.785CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion
title Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion
spellingShingle Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion
Benvenuto, Omar Gustavo
BINARIES: ECLIPSING
STARS: EARLY-TYPE
STARS: EVOLUTION
STARS: FUNDAMENTAL PARAMETERS
STARS: INDIVIDUAL: HD 93205
STARS: INTERIORS
title_short Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion
title_full Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion
title_fullStr Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion
title_full_unstemmed Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion
title_sort Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion
dc.creator.none.fl_str_mv Benvenuto, Omar Gustavo
Serenelli, A. M.
Althaus, Leandro Gabriel
Barba, Rodolfo Hector
Morrell, Nidia Irene
author Benvenuto, Omar Gustavo
author_facet Benvenuto, Omar Gustavo
Serenelli, A. M.
Althaus, Leandro Gabriel
Barba, Rodolfo Hector
Morrell, Nidia Irene
author_role author
author2 Serenelli, A. M.
Althaus, Leandro Gabriel
Barba, Rodolfo Hector
Morrell, Nidia Irene
author2_role author
author
author
author
dc.subject.none.fl_str_mv BINARIES: ECLIPSING
STARS: EARLY-TYPE
STARS: EVOLUTION
STARS: FUNDAMENTAL PARAMETERS
STARS: INDIVIDUAL: HD 93205
STARS: INTERIORS
topic BINARIES: ECLIPSING
STARS: EARLY-TYPE
STARS: EVOLUTION
STARS: FUNDAMENTAL PARAMETERS
STARS: INDIVIDUAL: HD 93205
STARS: INTERIORS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We present a method to calculate masses for components of both eclipsing and non-eclipsing binary systems as long as their apsidal motion rates are available. The method is based on the fact that the equation that gives the rate of apsidal motion is a supplementary equation that allows the computation of the masses of the components, if their radii and the internal structure constants can be obtained from theoretical models. For this reason the use of this equation makes the method presented here model dependent. We apply this method to calculate the mass of the components of the non-eclipsing massive binary system HD 93205 (O3 V + O8 V), which is suspected to be a very young system. To this end, we have computed a grid of evolutionary models covering the mass range of interest, and taking the mass of the primary (M1) as the only independent variable, we solve the equation of apsidal motion for M1 as a function of the age of the system. The mass of the primary that we find ranges from M1 = 60 ± 19 M⊙ for zero-age main-sequence models, which sets an upper limit for M1, down to M1 = 40 ± 9 M⊙ for an age of 2 Myr. Accordingly, the upper limit derived for the mass of the secondary (M2 = QM1) M2 = 25 M⊙ is in very good agreement with the masses derived for other O8 V stars occurring in eclipsing binaries.
Fil: Benvenuto, Omar Gustavo. 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
Fil: Serenelli, A. M.. Universidad Nacional de La Plata; Argentina
Fil: Althaus, Leandro Gabriel. 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
Fil: Barba, Rodolfo Hector. Universidad Nacional de La Plata; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Morrell, Nidia Irene. 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
description We present a method to calculate masses for components of both eclipsing and non-eclipsing binary systems as long as their apsidal motion rates are available. The method is based on the fact that the equation that gives the rate of apsidal motion is a supplementary equation that allows the computation of the masses of the components, if their radii and the internal structure constants can be obtained from theoretical models. For this reason the use of this equation makes the method presented here model dependent. We apply this method to calculate the mass of the components of the non-eclipsing massive binary system HD 93205 (O3 V + O8 V), which is suspected to be a very young system. To this end, we have computed a grid of evolutionary models covering the mass range of interest, and taking the mass of the primary (M1) as the only independent variable, we solve the equation of apsidal motion for M1 as a function of the age of the system. The mass of the primary that we find ranges from M1 = 60 ± 19 M⊙ for zero-age main-sequence models, which sets an upper limit for M1, down to M1 = 40 ± 9 M⊙ for an age of 2 Myr. Accordingly, the upper limit derived for the mass of the secondary (M2 = QM1) M2 = 25 M⊙ is in very good agreement with the masses derived for other O8 V stars occurring in eclipsing binaries.
publishDate 2002
dc.date.none.fl_str_mv 2002-02
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/11336/36895
Benvenuto, Omar Gustavo; Serenelli, A. M.; Althaus, Leandro Gabriel; Barba, Rodolfo Hector; Morrell, Nidia Irene; Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 330; 2; 2-2002; 435-442
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/36895
identifier_str_mv Benvenuto, Omar Gustavo; Serenelli, A. M.; Althaus, Leandro Gabriel; Barba, Rodolfo Hector; Morrell, Nidia Irene; Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 330; 2; 2-2002; 435-442
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://onlinelibrary.wiley.com/doi/10.1046/j.1365-8711.2002.05083.x/abstract
info:eu-repo/semantics/altIdentifier/doi/10.1046/j.1365-8711.2002.05083.x
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/330/2/435/1083947
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
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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 Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.070432

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