J/A+A/618/A79ivo://CDS.VizieR/J/A+A/618/A79doi:10.26093/cds/vizier.36180079CDSSiwak M.Winiarski M.Ogloza W.Drozdz M.Zola S.Moffat A.F.J.,Stachowski G.Rucinski S.M.Cameron C.Matthews J.M.Weiss W.W.,Kuschnig R.Rowe J.F.Guenther D.B.Sasselov D.2019-01-25T14:35:54Z2018-10-16T08:07:39ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frpre-main-sequence-starsvariable-starsphotometryWe investigate small-amplitude light variations in FU Ori occurring in timescales of days and weeks. We seek to determine the mechanisms that lead to these light changes. Methods. The visual light curve of FU Ori gathered by the MOST satellite continuously for 55 days in the 2013-2014 winter season and simultaneously obtained ground-based multi-colour data were compared with the results from a disc and star light synthesis model. Hotspots on the star are not responsible for the majority of observed light variations. Instead, we found that the long periodic family of 10.5-11.4d (presumably) quasi-periods showing light variations up to 0.07 mag may arise owing to the rotational revolution of disc inhomogeneities located between 16-20 solar radii. The same distance is obtained by assuming that these light variations arise because of a purely Keplerian revolution of these inhomogeneities for a stellar mass of 0.7 solar mass. The short-periodic (3-1.38d) small amplitude (0.01mag) light variations show a clear sign of period shortening, similar to what was discovered in the first MOST observations of FU Ori. Our data indicate that these short-periodic oscillations may arise because of changing visibility of plasma tongues (not included in our model), revolving in the magnetospheric gap and/or likely related hotspots as well. Results obtained for the long-periodic 10-11d family of light variations appear to be roughly in line with the colour-period relation, which assumes that longer periods are produced by more external and cooler parts of the disc. Coordinated observations in a broad spectral range are still necessary to fully understand the nature of the short-periodic 1-3d family of light variations and their period changes.2018A&A...618A..79Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/618/A79CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/618/A79https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/618/A79http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/618/A79https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/618/A79https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/618/A79http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/618/A79GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/618/A79/tablea1Original MOST pipeline result (Fig.1a)recnoRecord number assigned by the VizieR team. 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Should Not be used for identification.meta.recordintDateHelocentric Julian Date (HJD-2400000)dtime.epochdoublemagMagnitude in Band (1)magphot.magdoublee_magrms error on magmagstat.error;phot.magdoubleBandBand for magnitudeinstr.bandpasscharSystemInstrument or filter systemmeta.code;instr.filtercharJ/A+A/618/A79/tablea5*Mount Suhora Johnson V light curverecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDateHelocentric Julian Date (HJD-2400000)dtime.epochdoublemagMagnitude in Band (1)magphot.magdoublee_magrms error on magmagstat.error;phot.magdoubleBandBand for magnitudeinstr.bandpasscharSystemInstrument or filter systemmeta.code;instr.filtercharJ/A+A/618/A79/tablea3MOST light curve de-trended (orbital averages, Fig.1d and Fig.2)recnoRecord number assigned by the VizieR team. 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