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

Autores
Benvenuto, Omar Gustavo; Serenelli, Aldo Marcelo; Althaus, Leandro Gabriel; Barbá, Rodolfo Héctor; 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.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
Binaries: eclipsing
Stars: early-type
Stars: evolution
Stars: fundamental parameters
Stars: individual: HD 93205
Stars: interiors
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/84672

id SEDICI_7a0a10f2bba14dbd35ea55fc5c668b22
oai_identifier_str oai:sedici.unlp.edu.ar:10915/84672
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motionBenvenuto, Omar GustavoSerenelli, Aldo MarceloAlthaus, Leandro GabrielBarbá, Rodolfo HéctorMorrell, Nidia IreneCiencias AstronómicasBinaries: eclipsingStars: early-typeStars: evolutionStars: fundamental parametersStars: individual: HD 93205Stars: interiorsWe 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 <i>model dependent</i>. We apply this method to calculate the mass of the components of the <i>non-eclipsing</i> 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 (M<SUB>1</SUB>) 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 M<SUB>1</SUB> = 60 ± 19 M⊙ for zero-age main-sequence models, which sets an upper limit for M<SUB>1</SUB>, down to M1 = 40 ± 9 M⊙ for an age of 2 Myr. Accordingly, the upper limit derived for the mass of the secondary (M<SUB>2</SUB> = QM<SUB>1</SUB>) M<SUB>2</SUB> = 25 M⊙ is in very good agreement with the masses derived for other O8 V stars occurring in eclipsing binaries.Facultad de Ciencias Astronómicas y Geofísicas2002info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf435-442http://sedici.unlp.edu.ar/handle/10915/84672enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1046/j.1365-8711.2002.05083.xinfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:16Zoai:sedici.unlp.edu.ar:10915/84672Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:16.309SEDICI (UNLP) - Universidad Nacional de La Platafalse
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
Ciencias Astronómicas
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, Aldo Marcelo
Althaus, Leandro Gabriel
Barbá, Rodolfo Héctor
Morrell, Nidia Irene
author Benvenuto, Omar Gustavo
author_facet Benvenuto, Omar Gustavo
Serenelli, Aldo Marcelo
Althaus, Leandro Gabriel
Barbá, Rodolfo Héctor
Morrell, Nidia Irene
author_role author
author2 Serenelli, Aldo Marcelo
Althaus, Leandro Gabriel
Barbá, Rodolfo Héctor
Morrell, Nidia Irene
author2_role author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Binaries: eclipsing
Stars: early-type
Stars: evolution
Stars: fundamental parameters
Stars: individual: HD 93205
Stars: interiors
topic Ciencias Astronómicas
Binaries: eclipsing
Stars: early-type
Stars: evolution
Stars: fundamental parameters
Stars: individual: HD 93205
Stars: interiors
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 <i>model dependent</i>. We apply this method to calculate the mass of the components of the <i>non-eclipsing</i> 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 (M<SUB>1</SUB>) 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 M<SUB>1</SUB> = 60 ± 19 M⊙ for zero-age main-sequence models, which sets an upper limit for M<SUB>1</SUB>, down to M1 = 40 ± 9 M⊙ for an age of 2 Myr. Accordingly, the upper limit derived for the mass of the secondary (M<SUB>2</SUB> = QM<SUB>1</SUB>) M<SUB>2</SUB> = 25 M⊙ is in very good agreement with the masses derived for other O8 V stars occurring in eclipsing binaries.
Facultad de Ciencias Astronómicas y Geofísicas
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 <i>model dependent</i>. We apply this method to calculate the mass of the components of the <i>non-eclipsing</i> 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 (M<SUB>1</SUB>) 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 M<SUB>1</SUB> = 60 ± 19 M⊙ for zero-age main-sequence models, which sets an upper limit for M<SUB>1</SUB>, down to M1 = 40 ± 9 M⊙ for an age of 2 Myr. Accordingly, the upper limit derived for the mass of the secondary (M<SUB>2</SUB> = QM<SUB>1</SUB>) M<SUB>2</SUB> = 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
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
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://sedici.unlp.edu.ar/handle/10915/84672
url http://sedici.unlp.edu.ar/handle/10915/84672
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0035-8711
info:eu-repo/semantics/altIdentifier/doi/10.1046/j.1365-8711.2002.05083.x
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
435-442
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
_version_ 1844616035341172736
score 13.070432