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dc.contributor.authorRebull, L. M.
dc.contributor.authorStauffer, J. R.
dc.contributor.authorBouvier, J.
dc.contributor.authorCody, A. M.
dc.contributor.authorHillenbrand, L. A.
dc.contributor.authorSoderblom, D. R.
dc.contributor.authorValenti, J.
dc.contributor.authorBarrado, D.
dc.contributor.authorBouy, H.
dc.contributor.authorCiardi, D.
dc.contributor.authorPinsonneault, M.
dc.contributor.authorStassun, K.
dc.contributor.authorMicela, G.
dc.contributor.authorAigrain, S.
dc.contributor.authorVrba, F.
dc.contributor.authorSomers, G.
dc.contributor.authorGillen, E.
dc.contributor.authorCameron, A. Collier
dc.date.accessioned2016-09-06T16:32:00Z
dc.date.available2016-09-06T16:32:00Z
dc.date.issued2016-10-11
dc.identifier.citationRebull , L M , Stauffer , J R , Bouvier , J , Cody , A M , Hillenbrand , L A , Soderblom , D R , Valenti , J , Barrado , D , Bouy , H , Ciardi , D , Pinsonneault , M , Stassun , K , Micela , G , Aigrain , S , Vrba , F , Somers , G , Gillen , E & Cameron , A C 2016 , ' Rotation in the Pleiades with K 2. II. Multiperiod stars ' Astronomical Journal , vol. 152 , no. 5 , 114 . DOI: 10.3847/0004-6256/152/5/114en
dc.identifier.issn0004-6256
dc.identifier.otherPURE: 243386088
dc.identifier.otherPURE UUID: 977ddfe1-5710-474a-ab6b-c4e4a1b77978
dc.identifier.otherArXiv: http://arxiv.org/abs/1606.00055v1
dc.identifier.otherScopus: 84994667116
dc.identifier.urihttp://hdl.handle.net/10023/9451
dc.description.abstractWe use K2 to continue the exploration of the distribution of rotation periods in Pleiades that we began in Paper I. We have discovered complicated multi-period behavior in Pleiades stars using these K2 data, and we have grouped them into categories, which are the focal part of this paper. About 24% of the sample has multiple, real frequencies in the periodogram, sometimes manifesting as obvious beating in the light curves. Those having complex and/or structured periodogram peaks, unresolved multiple periods, and resolved close multiple periods are likely due to spot/spot group evolution and/or latitudinal differential rotation; these largely compose the slowly rotating sequence in P  versus (V−Ks)0 identified in Paper I. The fast sequence in P  versus (V−Ks)0 is dominated by single-period stars; these are likely to be rotating as solid bodies. Paper III continues the discussion, speculating about the origin and evolution of the period distribution in the Pleiades.en
dc.format.extent20en
dc.language.isoeng
dc.relation.ispartofAstronomical Journalen
dc.rights© 2016, American Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://dx.doi.org/10.3847/0004-6256/152/5/114en
dc.subjectGalaxies: clusters: individual (Pleiades)en
dc.subjectStars: rotationen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleRotation in the Pleiades with K2. II. Multiperiod starsen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.3847/0004-6256/152/5/114
dc.description.statusPeer revieweden


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