Open AccessPolar fields for AB Doradus
Author(s) -
McIvor T.,
Jardine M.,
Cameron A. Collier,
Wood K.,
Donati J.F.
Publication year - 2003
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2003.06986.x
Subject(s) - physics , polar , astrophysics , corona (planetary geology) , zeeman effect , radius , intermediate polar , solar prominence , magnetic field , stars , field (mathematics) , stellar magnetic field , astronomy , coronal mass ejection , white dwarf , solar wind , computer security , mathematics , quantum mechanics , astrobiology , pure mathematics , venus , computer science
Polar spots are often observed on rapidly‐rotating cool stars, but the nature of the magnetic field in these spots is as yet unknown. While Zeeman–Doppler imaging can provide surface magnetic field maps over much of the observed stellar surface, the Zeeman signature is suppressed in the dark polar regions. We have determined the effect on the global coronal structure of three current models for this polar field: that it is composed (a) of unipolar field, (b) of bipolar regions or (c) of nested rings of opposite polarity. We take as an example the young, rapid rotator AB Doradus ( P rot = 0.514 d) . By adding these model polar fields into the surface field maps determined from Zeeman–Doppler imaging, we have compared the resulting coronal structure with the observable properties of the corona – the magnitude and rotational modulation of the X‐ray emission measure and the presence of slingshot prominences trapped in the corona around the Keplerian corotation radius. We find that only the presence of a unipolar spot has any significant effect on the overall coronal structure, forcing much of the polar field to be open.