The cyclotron spectrum of VV Puppis

Details The cyclotron spectrum of VV Puppis The cyclotron spectrum of VV Puppis

Jan 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...189..325c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 189, no. 1-2, Jan. 1988, p. 325-330. Research supported by the Fundacao de Amp

Astronomy and Astrophysics

Astrophysics

13

Cyclotron Radiation, Stellar Magnetic Fields, Stellar Models, Stellar Spectra, White Dwarf Stars

Scientific paper

The authors examine whether a high temperature (⪆10 keV/kB) emission region is necessary to explain the width and height of the cyclotron spectrum of VV Puppis. They analyse the cyclotron spectrum using a model which takes into account, in particular, the variation with height of the magnetic field in the optical emission region of the accretion column (11.1%). The model also includes variations in density (9.3%), temperature (>100%), and diameter of the accretion column (6.1%). Using an emitting accretion column height of ≡0.04 Rwd, in agreement with observations (where Rwd is the white dwarf radius), the authors find good agreement with the width and height of the observed cyclotron lines, using 2.7 ≤ B ≤ 3.8×107gauss, and temperatures 0.2 ≤ T ≤ 2.5 keV/kB. The thickness of the emission region is s ≡ 5×107cm.

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