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| Main Authors: | , , , , |
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| Format: | Preprint |
| Published: |
2024
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2412.10932 |
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| _version_ | 1866915063827267584 |
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| author | Rodriguez, Luis F. Lizano, Susana Canto, Jorge Gonzalez, Ricardo F. Tapia, Mauricio |
| author_facet | Rodriguez, Luis F. Lizano, Susana Canto, Jorge Gonzalez, Ricardo F. Tapia, Mauricio |
| contents | We analyze the radio emission from the $β$ Cep star V2187 Cyg using archive data from the Jansky Very Large Array. The observations were made in ten epochs at 1.39 and 4.96 GHz in the highest angular resolution A configuration. We determine a spectral index of of $α= 0.6\pm0.2$ ($S_ν \propto ν^α$), consistent with an ionized wind or a partially optically-thick synchrotron or gyrosynchrotron source. The emission is spatially unresolved at both frequencies. The 4.96 GHz data shows a radio pulse with a duration of about one month that can be modeled in terms of an internal shock in the stellar wind produced by a sudden increase in the mass-loss rate and the terminal velocity. The quiescent radio emission of V2187 Cyg at 4.96 GHz (with a flux density of $\simeq 150~μJy$), cannot be explained in terms of an internally (by V2187 Cyg) or externally (by a nearby O star) photoionized wind. We conclude that, despite the spectral index suggestive of free-free emission from an ionized wind, the radio emission of V2187 Cyg most likely has a magnetic origin, a possibility that can be tested with a sensitive search for circular polarization in the radio, as expected from gyro-synchrotron radiation, and also by trying to measure the stellar magnetic field, that is expected to be in the range of several kGauss. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2412_10932 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Understanding the Radio Emission from the $β$ Cep star V2187 Cyg Rodriguez, Luis F. Lizano, Susana Canto, Jorge Gonzalez, Ricardo F. Tapia, Mauricio Solar and Stellar Astrophysics High Energy Astrophysical Phenomena We analyze the radio emission from the $β$ Cep star V2187 Cyg using archive data from the Jansky Very Large Array. The observations were made in ten epochs at 1.39 and 4.96 GHz in the highest angular resolution A configuration. We determine a spectral index of of $α= 0.6\pm0.2$ ($S_ν \propto ν^α$), consistent with an ionized wind or a partially optically-thick synchrotron or gyrosynchrotron source. The emission is spatially unresolved at both frequencies. The 4.96 GHz data shows a radio pulse with a duration of about one month that can be modeled in terms of an internal shock in the stellar wind produced by a sudden increase in the mass-loss rate and the terminal velocity. The quiescent radio emission of V2187 Cyg at 4.96 GHz (with a flux density of $\simeq 150~μJy$), cannot be explained in terms of an internally (by V2187 Cyg) or externally (by a nearby O star) photoionized wind. We conclude that, despite the spectral index suggestive of free-free emission from an ionized wind, the radio emission of V2187 Cyg most likely has a magnetic origin, a possibility that can be tested with a sensitive search for circular polarization in the radio, as expected from gyro-synchrotron radiation, and also by trying to measure the stellar magnetic field, that is expected to be in the range of several kGauss. |
| title | Understanding the Radio Emission from the $β$ Cep star V2187 Cyg |
| topic | Solar and Stellar Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2412.10932 |