Issue A&A Volume 463, Number 2, February IV 2007 Page(s) 647 - 655 Section Stellar structure and evolution DOI http://dx.doi.org/10.1051/0004-6361:20066332

A&A 463, 647-655 (2007)
DOI: 10.1051/0004-6361:20066332

Zeeman tomography of magnetic white dwarfs

IV. The complex field structure of the polars EF Eridani, BL Hydri and CP Tucanae

K. Beuermann¹, F. Euchner¹, K. Reinsch¹, S. Jordan², and B. T. Gänsicke<sup>3

1</sup>  Institut für Astrophysik, Universität Göttingen, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany
    e-mail: beuermann@astro.physik.uni-goettingen.de
²  Astronomisches Rechen-Institut am ZAH, Mönchhofstr. 12-14, 69120 Heidelberg, Germany
    e-mail: jordan@ari.uni-heidelberg.de
³  Department of Physics, University of Warwick, Coventry CV4 7AL, UK
    e-mail: Boris.Gaensicke@warwick.ac.uk

(Received 1 September 2006 / Accepted 26 September 2006 )

Abstract
Context. The magnetic fields of the accreting white dwarfs in magnetic cataclysmic variables (mCVs) determine the accretion geometries, the emission properties, and the secular evolution of these objects.
Aims.We determine the structure of the surface magnetic fields of the white dwarf primaries in magnetic CVs using Zeeman tomography.
Methods.Our study is based on orbital-phase resolved optical flux and circular polarization spectra of the polars EF Eri , BL Hyi , and CP Tuc obtained with FORS1 at the ESO VLT. An evolutionary algorithm is used to synthesize best fits to these spectra from an extensive database of pre-computed Zeeman spectra. The general approach has been described in previous papers of this series.
Results.The results achieved with simple geometries as centered or offset dipoles are not satisfactory. Significantly improved fits are obtained for multipole expansions that are truncated at degree l_</I>max=3 or 5 and include all tesseral and sectoral components with . The most frequent field strengths of 13, 18, and 10 MG for EF Eri , BL Hyi , and CP Tuc , and the ranges of field strength covered are similar for the dipole and multipole models, but only the latter provide access to accreting matter at the right locations on the white dwarf. The results suggest that the field geometries of the white dwarfs in short-period mCVs are quite complex, with strong contributions from multipoles higher than the dipole in spite of a typical age of the white dwarfs in CVs in excess of 1 Gyr.
Conclusions.It is feasible to derive the surface field structure of an accreting white dwarf from phase-resolved low-state circular spectropolarimetry of sufficiently high signal-to-noise ratio. The fact that independent information is available on the strength and direction of the field in the accretion spot from high-state observations helps in unraveling the global field structure.

Key words: stars: white dwarfs -- stars: magnetic fields -- stars: atmospheres -- polarization

© ESO 2007

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