Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion
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 computati...
| Autores: | , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2002 |
| País: | Argentina |
| Institución: | Consejo Nacional de Investigaciones Científicas y Técnicas |
| Repositorio: | CONICET Digital (CONICET) |
| Idioma: | inglés |
| OAI Identifier: | oai:ri.conicet.gov.ar:11336/36895 |
| Acceso en línea: | http://hdl.handle.net/11336/36895 |
| Access Level: | acceso abierto |
| Palabra clave: | BINARIES: ECLIPSING STARS: EARLY-TYPE STARS: EVOLUTION STARS: FUNDAMENTAL PARAMETERS STARS: INDIVIDUAL: HD 93205 STARS: INTERIORS https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| Sumario: | 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. |
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