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dc.contributor.authorBarnes, J R
dc.contributor.authorCollier Cameron, A
dc.contributor.authorJames, D J
dc.contributor.authorSteeghs, D
dc.date.accessioned2011-12-20T16:01:26Z
dc.date.available2011-12-20T16:01:26Z
dc.date.issued2001-09-21
dc.identifier.citationBarnes , J R , Collier Cameron , A , James , D J & Steeghs , D 2001 , ' Further images of α Persei G dwarfs ' Monthly Notices of the Royal Astronomical Society , vol. 326 , no. 3 , pp. 1057-1066 . https://doi.org/10.1046/j.1365-8711.2001.04648.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 494631
dc.identifier.otherPURE UUID: 91655773-c7e4-492a-86fc-69394df089f7
dc.identifier.otherWOS: 000171314400023
dc.identifier.otherScopus: 0000287509
dc.identifier.urihttp://hdl.handle.net/2299/7431
dc.description.abstractWe present two images of intermediate and low axial inclination G dwarfs (AP 149 and AP 193) in the young open cluster a Persei, and compare these with previous images of intermediate and high axial inclination objects in this cluster. All stars show starspots at high latitudes, with one star exhibiting a strong polar spot. Although low-latitude features are found on all stars to some degree, the detection of spots on AP 193 is marginal. The apparent difference in starspot morphology from one object to the next is probably the result of a stellar magnetic cycle, although the exact effect on the starspot distribution throughout a cycle is unknown. Polar spots are found in many Doppler images of rapidly rotating coot stars. In the past, their existence has been called into question, and it has been suggested that they could be the manifestations of NLTE (e.g. chromospheric filling in of line profiles) effects rather than real photospheric features. We assume the polar spots to be real photospheric features, and conclude that the flat-bottomed nature of the profile shape can be attributed to photospheric polar spots. The degree of truncation of the profile depends not only on spot size and strength, but also on the effective foreshortening of the polar region, a function of axial inclination. H alpha is in emission on AP 149 which shows a double peak at most phases. The time-series of the profile shows an s-wave pattern as the position of these peaks changes throughout the rotation cycle. We attribute this to coronal clouds located above the stellar surface in synchronous orbit. A maximum-entropy tomogram is derived revealing four distinct emission regions located near and above the corotation radius.en
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectline : profiles
dc.subjectstars : activity
dc.subjectstars : imaging
dc.subjectstars : late-type
dc.subjectstars : spots
dc.subjectSOLAR-TYPE STARS
dc.subjectSTELLAR SURFACE-STRUCTURE
dc.subjectMAIN-SEQUENCE STARS
dc.subjectDIFFERENTIAL ROTATION
dc.subjectANGULAR-MOMENTUM
dc.subjectDOPPLER IMAGES
dc.subjectCOOL STARS
dc.subjectPZ TEL
dc.subjectBD+22-DEGREES-4409
dc.subjectPERIODS
dc.titleFurther images of α Persei G dwarfsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
rioxxterms.versionofrecordhttps://doi.org/10.1046/j.1365-8711.2001.04648.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstyperestrictedAccess


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