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dc.contributor.authorStauffer, John
dc.contributor.authorRebull, Luisa
dc.contributor.authorDavid, Trevor
dc.contributor.authorJardine, Moira
dc.contributor.authorCollier Cameron, Andrew
dc.contributor.authorCody, Ann Marie
dc.contributor.authorHillenbrand, Lynne
dc.contributor.authorBarrado, David
dc.contributor.authorvan Eyken, Julian
dc.contributor.authorMelis, Carl
dc.contributor.authorBriceno, Cesar
dc.date.accessioned2018-01-23T15:30:12Z
dc.date.available2018-01-23T15:30:12Z
dc.date.issued2018-02
dc.identifier.citationStauffer , J , Rebull , L , David , T , Jardine , M , Collier Cameron , A , Cody , A M , Hillenbrand , L , Barrado , D , van Eyken , J , Melis , C & Briceno , C 2018 , ' More rapidly rotating PMS M dwarfs with light curves suggestive of orbiting clouds of material ' , Astronomical Journal , vol. 155 , no. 2 , 63 . https://doi.org/10.3847/1538-3881/aaa19den
dc.identifier.issn0004-6256
dc.identifier.otherPURE: 251818822
dc.identifier.otherPURE UUID: 2c4b78de-1a02-4eb9-9048-74de6339d83c
dc.identifier.otherBibCode: 2017arXiv171204390S
dc.identifier.otherScopus: 85042067837
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531468
dc.identifier.otherWOS: 000422902500001
dc.identifier.otherORCID: /0000-0002-1466-5236/work/57821887
dc.identifier.urihttp://hdl.handle.net/10023/12593
dc.description.abstractIn a previous paper, using data from K2 Campaign 2, we identified 11very low mass members of the ρ Oph and Upper Scorpius star-forming region as having periodic photometric variability and phased light curves showing multiple scallops or undulations. All the stars with the "scallop-shell" light curve morphology are mid-to-late M dwarfs without evidence of active accretion, and with photometric periods generally <1 day. Their phased light curves have too much structure to be attributed to non-axisymmetrically distributed photospheric spots and rotational modulation. We have now identified an additional eight probable members of the same star-forming region plus three stars in the Taurus star-forming region with this same light curve morphology and sharing the same period and spectral type range as the previous group. We describe the light curves of these new stars in detail and present their general physical characteristics. We also examine the properties of the overall set of stars in order to identify common features that might help elucidate the causes of their photometric variability.
dc.format.extent16
dc.language.isoeng
dc.relation.ispartofAstronomical Journalen
dc.rights© 2018, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at https://doi.org/10.3847/1538-3881/aaa19den
dc.subjectStars: pre-main sequenceen
dc.subjectStars: variables: T Tauri, Herbig Ae/Been
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleMore rapidly rotating PMS M dwarfs with light curves suggestive of orbiting clouds of materialen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
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.doihttps://doi.org/10.3847/1538-3881/aaa19d
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2017arXiv171204390Sen


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