Orbital period increase in ES Ceti
We report a long-term study of the eclipse times in the 10 minute helium binary ES Ceti. The binary period icreases rapidly, with with P/P = 6.2 x 106 years. This is consistent with the assumption that gravitational radiation (GR) drives the mass transfer, and it appears to be the first dynamical ev...
| Autores: | , , , , , , , |
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| Tipo de recurso: | artículo |
| Fecha de publicación: | 2018 |
| País: | España |
| Institución: | Universidad de Huelva (UHU) |
| Repositorio: | Arias Montano. Repositorio Institucional de la Universidad de Huelva |
| Idioma: | inglés |
| OAI Identifier: | oai:ariasmontano.uhu.es:10272/23097 |
| Acceso en línea: | https://hdl.handle.net/10272/23097 |
| Access Level: | acceso abierto |
| Palabra clave: | Accretion, accretion disks Binaries: close Novae, cataclysmic variables Stars: individual (ES Ceti) 21 Astronomía y Astrofísica |
| Sumario: | We report a long-term study of the eclipse times in the 10 minute helium binary ES Ceti. The binary period icreases rapidly, with with P/P = 6.2 x 106 years. This is consistent with the assumption that gravitational radiation (GR) drives the mass transfer, and it appears to be the first dynamical evidence that GR is indeed the driver of evolution in this class of very old cataclysmic variables -the AM Canum Venaticorum stars. |
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