1H 1752- AN ECLIPSING CATACLYSMIC VARIABLE WITH A SMALL ACCRETION DISK(081 )

We announce the discovery of an eclipsing nova-like cataclysmic variab le (CV) as the optical counterpart to the HEAO 1 X-ray source 1H1752+0 81. This CV has an orbital period of 1.882801 hr, a high equivalent wi dth of Hbeta, and an average m(V) of 16.4 out of eclipse. A geometric model is constructed from observations of the eclipse ingress and egre ss in many optical bandpasses. The broad-band emission originates prim arily in two regions; the disk/accretion stream ''hot spot'' and a com pact central component, which may be a spot on the white dwarf surface , the entire white dwarf surface or the boundary layer between the acc retion disk and the white dwarf surface. Based on the durations and of fsets of the two eclipses we determined the mass ratio q = 2.5 +/- 0.6 and the angle of inclination i = 77-degrees +/- 2-degrees. If the cen tral component is the entire white dwarf surface the masses of the sta rs are M1 = 0.80 +/- 0.06 M. and M2 = 0.32 +/- 0.06 M.. The disk is fa int and small (R(D) = 0.25 +/- 0.05 r(L1), where r(L1) is the distance from the primary to the L1 point), compared to other eclipsing CVs. T he small disk may result from the removal of angular momentum from the accretion disk by the magnetic field of the white dwarf; this CV may be a DQ Her type with a slowly rotating white dwarf. The emission-line velocities do not show the ''Z-wave'' expected from the eclipse of a Keplerian accretion disk, nor do they have the correct phasing to orig inate near the white dwarf. The most likely origin of the line emissio n is the hot spot. The secondary star is visible at wavelengths greate r-than-or-equal-to 6000 angstrom during eclipse. We estimate a spectra l type approximately M6 which, together with the observed m(I) = 16.94 during eclipse, results in a distance estimate of 150 +/- 27 pc.