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dc.contributor.authorRaetz, Stefanie
dc.contributor.authorStelzer, Beate
dc.contributor.authorScholz, Alexander
dc.date.accessioned2021-06-24T23:35:46Z
dc.date.available2021-06-24T23:35:46Z
dc.date.issued2020-08-27
dc.identifier268938802
dc.identifier9d05cf58-dbd8-45e8-9b0b-48cb8dea84c2
dc.identifier85087218091
dc.identifier000563771700007
dc.identifier.citationRaetz , S , Stelzer , B & Scholz , A 2020 , ' The rotation–activity relation of M dwarfs : from K2 to TESS and PLATO ' , Astronomische Nachrichten , vol. 341 , no. 5 , pp. 519-556 . https://doi.org/10.1002/asna.202013727en
dc.identifier.issn0004-6337
dc.identifier.otherRIS: urn:6723C317AE34892E73CCE01E030AB39C
dc.identifier.urihttps://hdl.handle.net/10023/23419
dc.description.abstractStudies of the rotation–activity relation of late‐type stars are essential to enhance our understanding of stellar dynamos and angular momentum evolution. We study the rotation–activity relation with K2 for M dwarfs, where it is especially poorly understood. We analyzed the light curves of all bright and nearby M dwarfs form the Superblink proper motion catalog that were in the K2 field of view. Using a sample of 430 M dwarfs observed in campaigns C0–C19 in long‐cadence mode, we determined the rotation period and a wealth of activity diagnostics. Our study of the rotation–activity relation based on photometric activity indicators confirmed the previously published abrupt change of the activity level at a rotation period of ∼10 days. Our sample, which is more than three times larger, increases the statistical significance of this finding.
dc.format.extent2462409
dc.language.isoeng
dc.relation.ispartofAstronomische Nachrichtenen
dc.subjectStars: late-typeen
dc.subjectStars: activityen
dc.subjectStars: rotationen
dc.subjectStars: flareen
dc.subjectQB Astronomyen
dc.subjectDASen
dc.subject.lccQBen
dc.titleThe rotation–activity relation of M dwarfs : from K2 to TESS and PLATOen
dc.typeJournal articleen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.identifier.doi10.1002/asna.202013727
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/2005.08688en


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