Abstract
Chemically peculiar (CP) stars of the upper main sequence are distant enough to permit us a relatively simplified approach to the problem of modelling their magnetic morphology. However, new observational techniques recently introduced by Mathys (1993) show that the common assumption of a‘quasi-dipolar’ field is too coarse an oversimplification. Although large-scale organised, the magnetic morphologies of CP stars exhibit a non axisymmetric and rather complex structure, which in some cases can be conveniently described in terms of the superposition of a dipole field and a quadrupole field. As a special example, I present a detailed model of a magnetic CP star, fully consistent with observations of Stokes I and V, Doppler broadening, and stellar radius.
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Bagnulo, S. (1999). Mapping Magnetic Fields of CP Stars from Stokes I and V Observations. In: Nagendra, K.N., Stenflo, J.O. (eds) Solar Polarization. Astrophysics and Space Science Library, vol 243. Springer, Dordrecht. https://doi.org/10.1007/978-94-015-9329-8_41
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DOI: https://doi.org/10.1007/978-94-015-9329-8_41
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