MOBSTER – VI. The crucial influence of rotation on the radio magnetospheres of hot stars
| Author(s) | Shultz, M. E. | |
| Author(s) | Owocki, S. P. | |
| Author(s) | ud-Doula, A. | |
| Author(s) | Biswas, A. | |
| Author(s) | Bohlender, D. | |
| Author(s) | Chandra, P. | |
| Author(s) | Das, B. | |
| Author(s) | David-Uraz, A. | |
| Author(s) | Khalack, V. | |
| Author(s) | Kochukhov, O. | |
| Author(s) | Landstreet, J. D. | |
| Author(s) | Leto, P. | |
| Author(s) | Monin, D. | |
| Author(s) | Neiner, C. | |
| Author(s) | Rivinius, Th. | |
| Author(s) | Wade, G. A. | |
| Date Accessioned | 2022-06-24T17:50:39Z | |
| Date Available | 2022-06-24T17:50:39Z | |
| Publication Date | 2022-04-27 | |
| Description | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. All rights reserved. The version of record is available at: https://doi.org/10.1093/mnras/stac136 | en_US |
| Abstract | Numerous magnetic hot stars exhibit gyrosynchrotron radio emission. The source electrons were previously thought to be accelerated to relativistic velocities in the current sheet formed in the middle magnetosphere by the wind opening magnetic field lines. However, a lack of dependence of radio luminosity on the wind power, and a strong dependence on rotation, has recently challenged this paradigm. We have collected all radio measurements of magnetic early-type stars available in the literature. When constraints on the magnetic field and/or the rotational period are not available, we have determined these using previously unpublished spectropolarimetric and photometric data. The result is the largest sample of magnetic stars with radio observations that has yet been analysed: 131 stars with rotational and magnetic constraints, of which 50 are radio-bright. We confirm an obvious dependence of gyrosynchrotron radiation on rotation, and furthermore find that accounting for rotation neatly separates stars with and without detected radio emission. There is a close correlation between H α emission strength and radio luminosity. These factors suggest that radio emission may be explained by the same mechanism responsible for H α emission from centrifugal magnetospheres, i.e. centrifugal breakout (CBO), however, while the H α-emitting magnetosphere probes the cool plasma before breakout, radio emission is a consequence of electrons accelerated in centrifugally driven magnetic reconnection. | en_US |
| Sponsor | The authors thank Dr. Stephen Drake for providing his unpublished radio measurements, which they hope have been put to good use. This work is based on observations obtained at the Canada-France- Hawaii Telescope ( CFHT ), which is operated by the National Research Council of Canada, the Institut National des Sciences de l’Univers (INSU) of the Centre National de la Recherche Scientifique (CNRS) of France, and the Univ ersity of Ha waii, and at the Obser- vatoire du Pic du Midi (France), operated by the INSU; and based on observations obtained at the Dominion Astrophysical Observatory, National Research Council Herzberg Astronomy and Astrophysics Research Centre, National Research Council of Canada. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes ( MAST ). Funding for the TESS mission is provided by NASA’s Science Mission directorate. We thank the staff of the GMRT that made the uGMRT observations possible. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. This work has made use of the VALD database, operated at Uppsala University, the Institute of Astronomy RAS in Moscow, and the University of Vienna. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. MES acknowledges the financial support provided by the Annie Jump Cannon Fellowship, supported by the University of Delaware and endowed by the Mount Cuba Astronomical Observatory. AuD acknowledges support by NASA through Chandra Award 26 number TM1-22001B issued by the Chandra X-ray Observatory 27 Center, which is operated by the Smithsonian Astrophysical Observatory for and behalf of NASA under contract NAS8-03060. VK acknowledges support by Natural Sciences and Engineering Research Council of Canada (NSERC). AB, BD, and PC acknowledge support of the Department of Atomic Energy, Go v ernment of India, under project no. 12-R&D-TFR-5.02-0700. GAW acknowledges Disco v ery Grant support from NSERC. JDL acknowledges support from NSERC, funding reference number 6377–2016. OK acknowledges support by the Swedish Research Council and the Swedish National Space Board. The material is based upon work supported by NASA under award number 80GSFC21M0002. | en_US |
| Citation | M E Shultz, S P Owocki, A ud-Doula, A Biswas, D Bohlender, P Chandra, B Das, A David-Uraz, V Khalack, O Kochukhov, J D Landstreet, P Leto, D Monin, C Neiner, Th Rivinius, G A Wade, MOBSTER – VI. The crucial influence of rotation on the radio magnetospheres of hot stars, Monthly Notices of the Royal Astronomical Society, Volume 513, Issue 1, June 2022, Pages 1429–1448, https://doi.org/10.1093/mnras/stac136 | en_US |
| ISSN | 1365-2966 | |
| URL | https://udspace.udel.edu/handle/19716/31029 | |
| Language | en_US | en_US |
| Publisher | Monthly Notices of the Royal Astronomical Society | en_US |
| Keywords | magnetic reconnection | en_US |
| Keywords | stars: early-type | en_US |
| Keywords | stars: magnetic fields | en_US |
| Keywords | stars: rotation | en_US |
| Keywords | radio continuum: stars | en_US |
| Title | MOBSTER – VI. The crucial influence of rotation on the radio magnetospheres of hot stars | en_US |
| Type | Article | en_US |
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