THE MAGNETIC-FIELD OF THE INTERMEDIATE POLAR RE-0751+14

Piirola, Hakala, & Coyne modeled the optical/IR light curve of RE 0751 +14 assuming a uniform shock structure and neglecting the hard X-ray e mission. In this paper, we model the light curves at optical/IR and ha rd X-ray wavelengths and include the effects of the shock structure. W e base our model on accretion onto a white dwarf with a displaced magn etic 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 sp in period largely determine the position of the emission regions. Furt hermore, the observed maximum X-ray flux constrains the specific accre tion 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 Pii rola et al. It had been proposed previously that there must exist asyn chronous rotators with sufficiently strong magnetic fields such that t he binaries will evolve into AM Her binaries (Chanmugam & Ray; King, F rank, & Ritter). With this deduced high magnetic field, RE 0751+14 is the most likely example of such a system known to date.