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The Magnetic Field of the Intermediate Polar RE 0751+14

Published online by Cambridge University Press:  12 April 2016

H. Väth
H. Väth*
Affiliation:
Institut für Astronomie und Astrophysik der Universität, 24098 Kiel, Germany([email protected])

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Piirola, Hakala & Coyne (1993) modeled the optical/IR light curve of RE 0751+14 assuming a uniform shock structure and neglecting the hard X-ray emission. In this paper, we model the light curves at optical/IR and hard X-ray wavelengths and include the effects of the shock structure.

We base our model on accretion onto a white dwarf with a displaced magnetic dipole for a range of likely white dwarf masses. We find that the observed intensity variations of X-rays and in the I band over one spin period largely determine the position of the emission regions. Furthermore, the observed maximum X-ray flux constrains the specific accretion rate. We deduce that the magnetic field at the pole is likely to be in the range 9 .. .21 MG, which is consistent with the estimates of Piirola et al. (1993). It had been proposed previously that there must exist asynchronous rotators with sufficiently strong magnetic fields such that the binaries will evolve into AM Her binaries (Chanmugam & Ray 1984; King, Frank & Ritter 1985). With this deduced high magnetic field RE 0751+14 is the most likely example of such a system known to date.

Type
Intermediate Polars
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 183
Copyright
Copyright © Kluwer 1996

References

Chanmugam, G., Ray, A., 1984, Ap. J., 285, 252 Google Scholar
King, A.R., Frank, J., Ritter, H., 1985, MNRAS, 213, 181 Google Scholar
Piirola, V., Hakala, P., Coyne, G.V., 1993, Ap. J., 410, L107 Google Scholar
Väth, H., Chanmugam, G., Frank, J., 1996, Ap. J., in pressGoogle Scholar