Circumbinary planets orbiting the rapidly pulsating subdwarf B-type binary NY Vir
We report here the tentative discovery of a Jovian planet in orbit around<br />the rapidly pulsating subdwarf B-type (sdB-type) eclipsing binary NY Vir. By using new determined eclipse times together those collected from the literature, we detect that the observed-calculated (O-C) curve of NY...
| Autores: | , , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2012 |
| País: | Argentina |
| Institución: | Consejo Nacional de Investigaciones Científicas y Técnicas |
| Repositorio: | CONICET Digital (CONICET) |
| Idioma: | inglés |
| OAI Identifier: | oai:ri.conicet.gov.ar:11336/42477 |
| Acceso en línea: | http://hdl.handle.net/11336/42477 |
| Access Level: | acceso abierto |
| Palabra clave: | Close binaries Eclipsing binaries NY VIR (estrella) Subdwarfs Planetary systems https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| Sumario: | We report here the tentative discovery of a Jovian planet in orbit around<br />the rapidly pulsating subdwarf B-type (sdB-type) eclipsing binary NY Vir. By using new determined eclipse times together those collected from the literature, we detect that the observed-calculated (O-C) curve of NY Vir shows a small-amplitude cyclic variation with a period of 7.9 years and a semiamplitude of 6.1 s, while it undergoes a downward parabolic change (revealing a period decrease at a rate of _dP/dt = -9.2 x 10^-12). The periodic variation was analyzed for the light-travel time effect via the presence of a third body. The mass of the tertiary companion was determined to be M3 sin i´ = 2.3(+/-0.3) MJupiter when a total mass of 0.60 Msun for NY Vir is adopted. This suggests that it most probably is a giant circumbinary planet orbiting NY Vir at a distance of about 3.3 astronomical units (AU). Since the rate of period decrease can not be explained by true angular momentum loss caused by gravitational radiation or/and magnetic braking, the observed downward parabolic change in the O-C diagram may be only a part of a long-period (longer than 15 years) cyclic variation, which may reveal the presence of another Jovian planet (about 2.5 MJupiter) in the system. |
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