The magnetic field of the intermediate polar re 0751 + 14

H. Väth, Christian-Albrechts-Universität zu Kiel
G. Chanmugam, Louisiana State University
J. Frank, Louisiana State University


Piirola, Hakala, & Coyne 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. 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; King, Frank, & Ritter). With this deduced high magnetic field, RE 0751 + 14 is the most likely example of such a system known to date. © 1996. The American Astronomical Society. All rights reserved.