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dc.contributor.authorBarnes, J R
dc.contributor.authorCollier Cameron, A
dc.contributor.authorJames, D J
dc.contributor.authorDonati, J F
dc.date.accessioned2011-12-20T16:01:28Z
dc.date.available2011-12-20T16:01:28Z
dc.date.issued2001-06-11
dc.identifier.citationBarnes , J R , Collier Cameron , A , James , D J & Donati , J F 2001 , ' Doppler images from dual-site observations of southern rapidly rotating stars - II. Starspot patterns and differential rotation on Speedy Mic ' , Monthly Notices of the Royal Astronomical Society , vol. 324 , no. 1 , pp. 231-242 . https://doi.org/10.1046/j.1365-8711.2001.04309.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 494693
dc.identifier.otherPURE UUID: 1e3fa58b-da2b-4902-b17e-30e70367a74c
dc.identifier.otherWOS: 000169352700028
dc.identifier.otherScopus: 0000199016
dc.identifier.urihttp://hdl.handle.net/2299/7432
dc.description.abstractWe have secured high spatial and temporal resolution spectra of the rapidly rotating K dwarf Speedy Mic (HD 197890) at two sites and a common epoch of observations. The 0.38-d axial rotation period and the V-band magnitude of 9.33 make it a difficult target for Doppler imaging. In order to obtain high signal-to-noise ratio profiles from 300-s exposures, we apply the technique of least-squares deconvolution to the large number of photospheric absorption lines available in each of our spectra. This allows us to derive high-resolution maximum-entropy-regularized Doppler images of the stellar surface. Using these techniques, we also derive radial velocities and accurate projected equatorial rotation velocities which are consistent to within similar to1 km s(-1) Our surface maps reveal one of the most heavily spotted photospheres seen on a rapid rotator, with starspots occurring at all latitudes, At the time of observations, Speedy Mic had no strong polar spot, but it shows spots concentrated in low- and intermediate-latitude bands. We attempt a differential rotation measurement, but lack of sufficient phase coverage allows determination of only a lower limit of 59 d for the time it takes the equatorial regions to lap the polar regions. We also find variations in the heavily filled-in Her line which can be attributed to prominences passing in front of the stellar disc. Despite the rapid rotation, the appearance of the same features on consecutive nights of observations shows the clouds to be stable on time-scales of at least a day.en
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectline : profiles
dc.subjectmethods : data analysis
dc.subjecttechniques : miscellaneous
dc.subjectstars : activity
dc.subjectstars : individual : Speedy Mic (HD 197890)
dc.subjectstars : late-type
dc.subjectMAIN-SEQUENCE STARS
dc.subjectSOLAR-TYPE STARS
dc.subjectLOW-MASS STARS
dc.subjectT-TAURI STARS
dc.subjectALPHA-PERSEI
dc.subjectAB DORADUS
dc.subjectACTIVE STARS
dc.subjectEVOLUTION
dc.subjectSPECTROSCOPY
dc.subjectPLEIADES
dc.titleDoppler images from dual-site observations of southern rapidly rotating stars - II. Starspot patterns and differential rotation on Speedy Micen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1046/j.1365-8711.2001.04309.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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