Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12666/509
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dc.rights.licensePublished 2021 January 11 © 2021. The American Astronomical Society. All rights reserved.-
dc.contributor.authorStauffer, J.-
dc.contributor.authorRebull, L. M.-
dc.contributor.authorJardine, M.-
dc.contributor.authorCollier Cameron, A.-
dc.contributor.authorCody, A. M.-
dc.contributor.authorHillenbrand, L. A.-
dc.contributor.authorBarrado, D.-
dc.contributor.authorKruse, E.-
dc.contributor.authorPowell, B. P.-
dc.date.accessioned2022-02-10T13:08:30Z-
dc.date.available2022-02-10T13:08:30Z-
dc.date.issued2021-01-11-
dc.identifier.citationThe Astronomical Journal 161(2): 60(2021)es
dc.identifier.issn0004-6256-
dc.identifier.otherhttps://iopscience.iop.org/article/10.3847/1538-3881/abc7c6-
dc.identifier.urihttp://hdl.handle.net/20.500.12666/509-
dc.description.abstractUsing K2, we recently discovered a new type of periodic photometric variability while analyzing the light curves of members of Upper Sco. The 23 exemplars of this new variability type are all mid-M dwarfs, with short rotation periods. Their phased light curves have one or more broad flux dips or multiple arcuate structures which are not explicable by photospheric spots or eclipses by solid bodies. Now, using Transiting Exoplanet Survey Satellite data, we have searched for this type of variability in the other major sections of Sco-Cen, Upper Centaurus-Lupus (UCL), and Lower Centaurus-Crux (LCC). We identify 28 stars with the same light curve morphologies. We find no obvious difference between the Upper Sco and the UCL/LCC representatives of this class in terms of their light curve morphologies, periods, or variability amplitudes. The physical mechanism behind this variability is unknown, but as a possible clue we show that the rapidly rotating mid-M dwarfs in UCL/LCC have slightly different colors from the slowly rotating M dwarfs—they either have a blue excess (hot spots?) or a red excess (warm dust?). One of the newly identified stars (TIC242407571) has a very striking light curve morphology. At about every 0.05 in phase are features that resemble icicles. The icicles arise because there is a second periodic system whose main feature is a broad flux dip. Using a toy model, we show that the observed light curve morphology results only if the ratio of the two periods and the flux-dip width are carefully arranged.es
dc.description.sponsorshipSome of the data presented in this paper were obtained from MAST. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This research has made use of the NASA/IPAC Infrared Science Archive (IRSA), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of NASA's Astrophysics Data System (ADS) Abstract Service, and of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of data products from 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation. The 2MASS data are served by the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication makes use of data products from WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.es
dc.language.isoenges
dc.publisherIOP Science Publishinges
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/4.0/-
dc.subjectYoung Stars Clusterses
dc.subjectM Starses
dc.subjectStellar Rotationes
dc.titleEven More Rapidly Rotating Pre-main-sequence M Dwarfs with Highly Structured Light Curves: An Initial Survey in the Lower Centaurus-Crux and Upper Centaurus-Lupus Associationses
dc.typeinfo:eu-repo/semantics/articlees
dc.contributor.orcid0000-0003-3595-7382-
dc.contributor.orcid0000-0001-6381-515X-
dc.contributor.orcid0000-0002-1466-5236-
dc.contributor.orcid0000-0002-8863-7828-
dc.contributor.orcid0000-0002-3656-6706-
dc.contributor.orcid0000-0002-5971-9242-
dc.contributor.orcid0000-0002-0493-1342-
dc.contributor.orcid0000-0003-0501-2636-
dc.identifier.doi10.3847/1538-3881/abc7c6-
dc.identifier.e-issn1538-3881-
dc.contributor.funderNational Aeronautics and Space Administration (NASA)-
dc.description.peerreviewedPeerreviewes
dc.identifier.funderhttp://dx.doi.org/10.13039/100000104-
dc.type.hasVersioninfo:eu-repo/semantics/publishedVersion-
dc.rights.accessRightsinfo:eu-repo/semantics/openAccess-
dc.type.coarhttp://purl.org/coar/resource_type/c_6501-
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