Studying stellar spin-down with Zeeman–Doppler magnetograms
Article
Article Title | Studying stellar spin-down with Zeeman–Doppler magnetograms |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | See, V. (Author), Jardine, M. (Author), Vidotto, A. A. (Author), Donati, J-F. (Author), Boro Saikia, S. (Author), Fares, R. (Author), Folsom, C. P. (Author), Hebrard, E. M. (Author), Jeffers, S. V. (Author), Marsden, S. C. (Author), Morin, J. (Author), Petit, P. (Author) and Waite, I. A. (Author) |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 466 (2), pp. 1542-1554 |
Number of Pages | 13 |
Year | 2017 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1093/mnras/stw3094 |
Web Address (URL) | https://academic.oup.com/mnras/article/466/2/1542/2617722 |
Abstract | Magnetic activity and rotation are known to be intimately linked for low-mass stars. Understanding rotation evolution over the stellar lifetime is therefore an important goal within stellar astrophysics. In recent years, there has been increased focus on how the complexity of the stellar magnetic field affects the rate of angular-momentum loss from a star. This is a topic that Zeeman–Doppler imaging (ZDI), a technique that is capable of reconstructing the large-scale magnetic field topology of a star, can uniquely address. Using a potential field source surface model, we estimate the open flux, mass-loss rate and angular-momentum-loss rates for a sample of 66 stars that have been mapped with ZDI. We show that the open flux of a star is predominantly determined by the dipolar component of its magnetic field for our choice of source surface radius. We also show that, on the main sequence, the open flux, mass loss and angular-momentum-loss rates increase with decreasing Rossby number. The exception to this rule is stars less massive than 0.3Msun. Previous work suggests that low-mass M dwarfs may possess either strong, ordered and dipolar fields or weak and complex fields. This range of field strengths results in a large spread of angular momentum-loss rates for these stars and has important consequences for their spin-down behaviour. Additionally, our models do not predict a transition in the mass-loss rates at the so-called wind-dividing line noted from Lyα studies. |
Keywords | polarimetric, stars, evolution, magnetic field, rotation |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
Public Notes | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
Byline Affiliations | University of St Andrews, United Kingdom |
University of Dublin, Ireland | |
University of Toulouse, France | |
Georg August University of Gottingen, Germany | |
National Institute of Astrophysics, Italy | |
York University, Canada | |
University of Gottingen, Germany | |
Computational Engineering and Science Research Centre | |
Montpellier Universe and Particles Laboratory, France | |
Institution of Origin | University of Southern Queensland |
https://research.usq.edu.au/item/q488w/studying-stellar-spin-down-with-zeeman-doppler-magnetograms
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