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Influence of magnetic cycles on stellar prominences and their mass loss rates

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Faller_2022_MNRAS_Influence_of_magnetic_cycles_AAM.pdf (7.057Mb)
Date
07/2022
Author
Faller, Sarah J
Jardine, Moira M
Funder
Science & Technology Facilities Council
Grant ID
ST/R00824/1
Keywords
Stars: solar-type
Stars: magnetic field
Stars: mass-loss
QB Astronomy
QC Physics
DAS
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Abstract
Observations of rapidly-rotating cool stars often show coronal “slingshot” prominences that remove mass and angular momentum when they are ejected. The derived masses of these prominences show a scatter of some two orders of magnitude. In order to investigate if this scatter could be intrinsic, we use a full magnetic cycle of solar magnetograms to model the coronal structure and prominence distribution in a young Sun, where we scale the field strength in the magnetograms with angular velocity according to B∝Ω−1.32. We reproduce both the observed prominence masses and their scatter. We show that both the field strength and the field geometry contribute to the prominence masses that can be supported and to the rate at which they are ejected. Predicted prominence masses follow the magnetic cycle, but with half the period, peaking both at cycle maximum and at cycle minimum. We show that mass loss rates in prominences are less than those predicted for the stellar wind. We also investigate the role of small-scale field that may be unresolved in typical stellar magnetograms. This provides only a small reduction in the predicted total prominence mass, principally by reducing the number of large magnetic loops that can support slingshot prominences. We conclude that the observed scatter in prominence masses can be explained by underlying magnetic cycles.
Citation
Faller , S J & Jardine , M M 2022 , ' Influence of magnetic cycles on stellar prominences and their mass loss rates ' , Monthly Notices of the Royal Astronomical Society , vol. 513 , no. 4 , pp. 5611–5620 . https://doi.org/10.1093/mnras/stac1273
Publication
Monthly Notices of the Royal Astronomical Society
Status
Peer reviewed
DOI
https://doi.org/10.1093/mnras/stac1273
ISSN
0035-8711
Type
Journal article
Rights
Copyright © 2022 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1093/mnras/stac1273.
Description
Funding: The authors acknowledge support from STFC consolidated grant number ST/R000824/1.
Collections
  • University of St Andrews Research
URI
http://hdl.handle.net/10023/25379

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