The winds of young Solar-type stars in the Pleiades, AB Doradus, Columba, and β Pictoris
Article
Evensberget, D, Marsden, S C, Carter, B D, Salmeron, R, Vidotto, A A, Folsom, C P, Kavanagh, R D, Pineda, J S, Driessen, F A and Strickert, K M. 2023. "The winds of young Solar-type stars in the Pleiades, AB Doradus, Columba, and β Pictoris
." Monthly Notices of the Royal Astronomical Society. 524 (2), pp. 2042-2063. https://doi.org/10.1093/mnras/stad1650
Article Title | The winds of young Solar-type stars in the Pleiades, AB Doradus, Columba, and β Pictoris |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | Evensberget, D, Marsden, S C, Carter, B D, Salmeron, R, Vidotto, A A, Folsom, C P, Kavanagh, R D, Pineda, J S, Driessen, F A and Strickert, K M |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 524 (2), pp. 2042-2063 |
Number of Pages | 22 |
Year | 2023 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1093/mnras/stad1650 |
Web Address (URL) | https://academic.oup.com/mnras/article/524/2/2042/7189907 |
Abstract | Solar-type stars, which shed angular momentum via magnetized stellar winds, enter the main sequence with a wide range of rotational periods P rot . This initially wide range of rotational periods contracts and has mostly vanished by a stellar age t ? 0 . 6 Gyr , after which Solar-type stars spin according to the Skumanich relation P rot ? ? t . Magnetohydrodynamic stellar wind models can impro v e our understanding of this convergence of rotation periods. We present wind models of 15 young Solar-type stars aged ?24 Myr to ?0.13 Gyr. With our previous wind models of stars aged ?0.26 and ?0.6 Gyr we obtain 30 consistent three-dimensional wind models of stars mapped with Zeeman-Doppler imaging - the largest such set to date. The models provide good cover of the pre-Skumanich phase of stellar spin-down in terms of rotation, magnetic field, and age. We find the mass-loss rate M ? ? 0. 9 ±0.1 with a residual spread of ?150 per cent and the wind angular momentum loss rate J? P -1 rot ? 1 . 3 ±0 . 2 with a residual spread of ?500 per cent where ? is the unsigned surface magnetic flux. When comparing different magnetic field scalings for each single star we find a gradual reduction in the power-law exponent with increasing magnetic field strength. |
Keywords | outflows |
Contains Sensitive Content | Does not contain sensitive content |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
Byline Affiliations | Centre for Astrophysics |
Leiden University, Netherlands | |
University of Tartu, Estonia | |
Netherlands Institute for Radio Astronomy, Netherlands | |
University of Colorado Boulder, United States |
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