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dc.contributor.authorXiang, Y.
dc.contributor.authorGu, S.-H.
dc.contributor.authorCollier Cameron, A.
dc.contributor.authorBarnes, J.R.
dc.date.accessioned2014-09-09T11:31:03Z
dc.date.available2014-09-09T11:31:03Z
dc.date.issued2014-03-01
dc.identifier.citationXiang , Y , Gu , S-H , Collier Cameron , A & Barnes , J R 2014 , ' Distribution and evolution of starspots on the RS CVn binary II Pegasi in 2004 ' , Monthly Notices of the Royal Astronomical Society , vol. 438 , no. 3 , pp. 2307-2316 . https://doi.org/10.1093/mnras/stt2345en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 146987584
dc.identifier.otherPURE UUID: 3c9a1de8-7285-4aac-97b1-6040f0c1ee3b
dc.identifier.otherScopus: 84894033579
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531446
dc.identifier.otherWOS: 000331877000024
dc.identifier.urihttp://hdl.handle.net/10023/5392
dc.descriptionThis work is supported by National Natural Science Foundation of China through grants Nos. 10373023, 10773027 and 11333006, Chinese Academy of Sciences through project KJCX2-YW-T24.en
dc.description.abstractWe present Doppler images of RS CVn-type binary II Peg based on two data sets obtained in 2004 February and November. In order to improve signal-to-noise ratio and reliability,we apply least-squares deconvolution technique to calculate average profiles from 2032 photospheric absorption lines. Both of the resulting surface images show a wide latitude distribution of starspots. Most spots are concentrated at a high-latitude belt above 60° and a low-latitude belt near equator. The starspots evolved dramatically between two observing runs, which may indicate shorter time-scale evolution in this epoch, especially for low-latitude belt. There is no stable preferred active longitude that can be found in our images. We also find out a possible phenomenon that the intermediate-latitude spot migrated poleward and merged with the high-latitude spot to make it stronger, which may reveal a more complex behaviour of starspots on II Peg. A potential change of orbital ephemeris zero-point was detected. This may imply an orbital period change of II Peg like other active close binaries.
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Societyen
dc.subjectStars: activityen
dc.subjectBinaries: closeen
dc.subjectStars: imagingen
dc.subjectStars: individual: II Pegen
dc.subjectStarspotsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleDistribution and evolution of starspots on the RS CVn binary II Pegasi in 2004en
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stt2345
dc.description.statusPeer revieweden


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