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
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/84672
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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 |
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openAccess |
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http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
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