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dc.contributor.authorFaller, Sarah J
dc.contributor.authorJardine, Moira M
dc.identifier.citationFaller , 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 .
dc.identifier.otherPURE: 279615289
dc.identifier.otherPURE UUID: 2aa299a5-b086-4b7a-9b67-91f11f44dc0d
dc.identifier.otherBibtex: 10.1093/mnras/stac1273
dc.identifier.otherORCID: /0000-0002-1466-5236/work/113398992
dc.identifier.otherScopus: 85133577227
dc.identifier.otherWOS: 000804922700009
dc.descriptionFunding: The authors acknowledge support from STFC consolidated grant number ST/R000824/1.en
dc.description.abstractObservations 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.
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 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
dc.subjectStars: solar-typeen
dc.subjectStars: magnetic fielden
dc.subjectStars: mass-lossen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleInfluence of magnetic cycles on stellar prominences and their mass loss ratesen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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