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dc.contributor.advisorCameron, A. C.
dc.contributor.authorPointer, Graham Richard
dc.coverage.spatialxiii, 105 p.en_US
dc.date.accessioned2018-03-14T14:08:59Z
dc.date.available2018-03-14T14:08:59Z
dc.date.issued2001
dc.identifier.urihttp://hdl.handle.net/10023/12940
dc.description.abstractObservations of AB Doradus, a nearby, rapidly-rotating K0 dwarf are analysed, and the surface magnetic field is shown to be approximated by a potential field. Evolving the surface magnetic field according to diffusion and the observed differential rotation still yields good correlation between the calculated and observed radial field after 30 days, contradictory to the results of Barnes et al. (1998), leading to the conclusion that there is an additional cause for the evolution of the magnetic field. The chromospheric magnetic field is modelled as a potential field with a source surface. Using the stability criteria g.B = 0 and B.V(g.B) < 0, places where prominences can be stable are investigated. For agreement with the results of Donati et al. (2000)- that prominences form preferentially near the equatorial plane and at and beyond corotation- it is necessary to add a quasidipolar field of maximum strength ~20G.en_US
dc.language.isoenen_US
dc.publisherUniversity of St Andrews
dc.subject.lccQB843.D9P7
dc.subject.lcshDwarf stars.en
dc.subject.lcshStars--Magnetic fields.en
dc.titleThe magnetic field of AB Doradûsen_US
dc.typeThesisen_US
dc.type.qualificationlevelDoctoralen_US
dc.type.qualificationnamePhD Doctor of Philosophyen_US
dc.publisher.institutionThe University of St Andrewsen_US


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