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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.urihttps://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.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorPPARC - Now STFCen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
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
dc.identifier.grantnumberST/J001651/1en
dc.identifier.grantnumberST/I000666/1en
dc.identifier.grantnumberPP/D000890/1en
dc.identifier.grantnumberST/G001006/1en
dc.identifier.grantnumberPP/F000065/1en


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