The solar wind in time – II. 3D stellar wind structure and radio emission
Article
Article Title | The solar wind in time – II. 3D stellar wind structure and radio emission |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | O Fionnagain, D. (Author), Vidotto, A. A. (Author), Petit, P. (Author), Folsom, C. P. (Author), Jeffers, S. V. (Author), Marsden, S. C. (Author), Morin, J. (Author), do Nascimento, Jr., J.-D. (Author) and BCool Collaboration, . (Author) |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 483 (1), pp. 873-886 |
Number of Pages | 14 |
Year | 2019 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1093/mnras/sty3132 |
Web Address (URL) | https://academic.oup.com/mnras/article/483/1/873/5199230 |
Abstract | In this work, we simulate the evolution of the solar wind along its main-sequence lifetime and compute its thermal radio emission. To study the evolution of the solar wind, we use a sample of solar mass stars at different ages. All these stars have observationally reconstructed magnetic maps, which are incorporated in our 3D magnetohydrodynamic simulations of their winds. We show that angular-momentum loss and mass-loss rates decrease steadily on evolutionary time-scales, although they can vary in a magnetic cycle time-scale. Stellar winds are known to emit radiation in the form of thermal bremsstrahlung in the radio spectrum. To calculate the expected radio fluxes from these winds, we solve the radiative transfer equation numerically from first principles. We compute continuum spectra across the frequency range 100 MHz to 100 GHz and find maximum radio flux densities ranging from 0.05 to 2.2 μJy. At a frequency of 1 GHz and a normalized distance of d = 10 pc, the radio flux density follows 0.24 (Ω/Ω☉)0.9 (d/[10pc])-2μJy, where Ω is the rotation rate. This means that the best candidates for stellar wind observations in the radio regime are faster rotators within distances of 10 pc, such as κ1 Ceti (0.73 μJy) and χ1 Ori (2.2 μJy). These flux predictions provide a guide to observing solar-type stars across the frequency range 0.1-100 GHz in the future using the next generation of radio telescopes, such as ngVLA and Square Kilometre Array. |
Keywords | stars: solar-type; stars: winds; outflows; radio continuum; stars |
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 ©: 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
Byline Affiliations | University of Dublin, Ireland |
University of Toulouse, France | |
Georg August University of Gottingen, Germany | |
Centre for Astrophysics | |
University of Montpellier, France | |
Federal University of Rio Grande do Norte, Brazil | |
Bernard Lyot Telescope, France | |
Institution of Origin | University of Southern Queensland |
https://research.usq.edu.au/item/q5724/the-solar-wind-in-time-ii-3d-stellar-wind-structure-and-radio-emission
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