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dc.contributor.authorStauffer, John
dc.contributor.authorRebull, Luisa
dc.contributor.authorBouvier, Jerome
dc.contributor.authorHillenbrand, Lynne A.
dc.contributor.authorCollier Cameron, Andrew
dc.contributor.authorPinsonneault, Marc
dc.contributor.authorAigrain, Suzanne
dc.contributor.authorBarrado, David
dc.contributor.authorBouy, Herve
dc.contributor.authorCiardi, David
dc.contributor.authorCody, Ann Marie
dc.contributor.authorDavid, Trevor
dc.contributor.authorMicela, Giusi
dc.contributor.authorSoderblom, David
dc.contributor.authorSomers, Garrett
dc.contributor.authorStassun, Keivan G.
dc.contributor.authorValenti, Jeff
dc.contributor.authorVrba, Frederick J.
dc.date.accessioned2016-09-06T15:31:35Z
dc.date.available2016-09-06T15:31:35Z
dc.date.issued2016-10-11
dc.identifier.citationStauffer , J , Rebull , L , Bouvier , J , Hillenbrand , L A , Collier Cameron , A , Pinsonneault , M , Aigrain , S , Barrado , D , Bouy , H , Ciardi , D , Cody , A M , David , T , Micela , G , Soderblom , D , Somers , G , Stassun , K G , Valenti , J & Vrba , F J 2016 , ' Rotation in the Pleiades with K 2. III. Speculations on origins and evolution ' Astronomical Journal , vol. 152 , no. 5 , 115 . https://doi.org/10.3847/0004-6256/152/5/115en
dc.identifier.issn0004-6256
dc.identifier.otherPURE: 243386131
dc.identifier.otherPURE UUID: 4ed2b526-b364-4159-b887-8b238e7836c7
dc.identifier.otherArXiv: http://arxiv.org/abs/1606.00057v2
dc.identifier.otherScopus: 84994627640
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531389
dc.identifier.urihttp://hdl.handle.net/10023/9448
dc.description.abstractWe use high quality K2 light curves for hundreds of stars in the Pleiades to understand better the angular momentum evolution and magnetic dynamos of young, low mass stars. The K2 light curves provide not only rotational periods but also detailed information from the shape of the phased light curve not available in previous studies. A slowly rotating sequence begins at (V−Ks)0 ∼ 1.1 (spectral type F5) and ends at (V−Ks)0 ∼ 3.7 (spectral type K8), with periods rising from ∼2 to ∼11 days in that interval. 52% percent of the Pleiades members in that color interval have periods within 30% of a curve defining the slow sequence; the slowly rotating fraction decreases significantly redward of (V−Ks)0=2.6. Nearly all of the slow-sequence stars show light curves that evolve significantly on timescales less than the K2 campaign duration. The majority of the FGK Pleiades members identified as photometric binaries are relatively rapidly rotating, perhaps because binarity inhibits star-disk angular momentum loss mechanisms during pre-main sequence evolution. The fully convective, late M dwarf Pleiades members (5.0 < (V−Ks)0 < 6.0) nearly always show stable light curves, with little spot evolution or evidence of differential rotation. During PMS evolution from ∼3 Myr (NGC2264 age) to ∼125 Myr (Pleiades age), stars of 0.3 M⊙ shed about half their angular momentum, with the fractional change in period between 3 and 125 Myr being nearly independent of mass for fully convective stars. Our data also suggest that very low mass binaries form with rotation periods more similar to each other and faster than would be true if drawn at random from the parent population of single stars.
dc.format.extent22
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/10.3847/0004-6256/152/5/115en
dc.subjectOpen clusters and associations: 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. III. Speculations on origins and evolutionen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.3847/0004-6256/152/5/115
dc.description.statusPeer revieweden


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