PERIODIC RADIO CONTINUUM EMISSION ASSOCIATED WITH THE β CEPHEI STAR V2187 CYG
We present new optical time-resolved photometry and medium-resolution spectroscopy of V2187 Cyg. We confirm its classification as a β Cephei star based on sinusoidal light variations with a period of 0.2539 days and mean amplitudes of 0.037 and 0.042 magnitudes in i and V , respectively. We classifi...
| Autores: | , , , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2014 |
| País: | México |
| Institución: | Universidad Nacional Autónoma de México |
| Repositorio: | Redalyc-UNAM |
| OAI Identifier: | oai:redalyc.org:57131044015 |
| Acceso en línea: | https://www.redalyc.org/articulo.oa?id=57131044015 |
| Access Level: | acceso abierto |
| Palabra clave: | Física, Astronomía y Matemáticas β Cephei) stars — stars Radio continuum individual (V1287 Cyg |
| Sumario: | We present new optical time-resolved photometry and medium-resolution spectroscopy of V2187 Cyg. We confirm its classification as a β Cephei star based on sinusoidal light variations with a period of 0.2539 days and mean amplitudes of 0.037 and 0.042 magnitudes in i and V , respectively. We classified the spectrum of this star as B2-3 V with no evidence of variations in the profiles of its absorption lines in timescales of hours or days. The stellar spectrum is totally absent of emis- sion lines. We detected unexpected faint radio continuum emission (between 0.4 and 0.8 mJy at 6-cm) showing a sinusoidal variation with a period of 12.8 days. The radio spectrum is thermal. We searched in the Very Large Array archive for radio continuum emission toward 15 other β Cephei stars. None of these additional stars, some of them much closer to the Sun than V2187 Cyg, was detected, indicating that radio emission from β Cephei stars is extremely uncommon. |
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