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Rotation in the Pleiades with K2. II. Multiperiod stars
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dc.contributor.author | Rebull, L. M. | |
dc.contributor.author | Stauffer, J. R. | |
dc.contributor.author | Bouvier, J. | |
dc.contributor.author | Cody, A. M. | |
dc.contributor.author | Hillenbrand, L. A. | |
dc.contributor.author | Soderblom, D. R. | |
dc.contributor.author | Valenti, J. | |
dc.contributor.author | Barrado, D. | |
dc.contributor.author | Bouy, H. | |
dc.contributor.author | Ciardi, D. | |
dc.contributor.author | Pinsonneault, M. | |
dc.contributor.author | Stassun, K. | |
dc.contributor.author | Micela, G. | |
dc.contributor.author | Aigrain, S. | |
dc.contributor.author | Vrba, F. | |
dc.contributor.author | Somers, G. | |
dc.contributor.author | Gillen, E. | |
dc.contributor.author | Cameron, A. Collier | |
dc.date.accessioned | 2016-09-06T16:32:00Z | |
dc.date.available | 2016-09-06T16:32:00Z | |
dc.date.issued | 2016-10-11 | |
dc.identifier | 243386088 | |
dc.identifier | 977ddfe1-5710-474a-ab6b-c4e4a1b77978 | |
dc.identifier | 84994667116 | |
dc.identifier | 000386139400002 | |
dc.identifier.citation | Rebull , 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 . https://doi.org/10.3847/0004-6256/152/5/114 | en |
dc.identifier.issn | 0004-6256 | |
dc.identifier.other | ArXiv: http://arxiv.org/abs/1606.00055v1 | |
dc.identifier.other | ORCID: /0000-0002-8863-7828/work/58531439 | |
dc.identifier.uri | https://hdl.handle.net/10023/9451 | |
dc.description.abstract | We 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. | |
dc.format.extent | 20 | |
dc.format.extent | 4257724 | |
dc.language.iso | eng | |
dc.relation.ispartof | Astronomical Journal | en |
dc.subject | Galaxies: clusters: individual (Pleiades) | en |
dc.subject | Stars: rotation | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | NDAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | Rotation in the Pleiades with K2. II. Multiperiod stars | en |
dc.type | Journal article | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.identifier.doi | https://doi.org/10.3847/0004-6256/152/5/114 | |
dc.description.status | Peer reviewed | en |
dc.identifier.grantnumber | ST/M001296/1 | en |
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