Superhumps and spin-period variations in the intermediate polar RX J2133.7+5107
We report the results of long-term time series photometry on RX J2133.7+5107, an intermediate polar distinguished by its long orbital period (7.14 h) and rapid rotation (571 s) of its white dwarf. The light curves show the presence of a conspicuous modulation with a 6.72-h period, 6.1 ± 0.1 per cent...
| Autores: | , , |
|---|---|
| Tipo de recurso: | artículo |
| Fecha de publicación: | 2017 |
| 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:10272/15274 |
| Acceso en línea: | http://hdl.handle.net/10272/15274 |
| Access Level: | acceso abierto |
| Palabra clave: | Accretion Accretion discs Binaries Close Stars Individual RX J2133.7+5107 Novae Cataclysmic variables |
| Sumario: | We report the results of long-term time series photometry on RX J2133.7+5107, an intermediate polar distinguished by its long orbital period (7.14 h) and rapid rotation (571 s) of its white dwarf. The light curves show the presence of a conspicuous modulation with a 6.72-h period, 6.1 ± 0.1 per cent shorter than the orbital period, which we interpret as a (negative) superhump associated with the nodal precession of the accretion disc. This detection may prove a challenge to the idea that superhumps are limited to binaries of short orbital period. Our rotational timings over the 7 yr spanned by our observations show spin-up at a rate of 3.41(2) ms yr-1 or, equivalently, on a time-scale |P/P?|=0.17×106 yr. The latter is sensibly shorter than the time-scale of spin period variations reported for other intermediate polars, possibly due to a greater accretion rate. |
|---|