THE NOVA-LIKE CATACLYSMIC VARIABLE-STAR - KUV-0859+415

KUV 0859 + 415 has been found to be an eclipsing, nova-like cataclysmi c variable with an orbital period of 3 h and 40 min. We find that it d iffers from other eclipsing systems of similar period (sometimes calle d the SW Sex stars) in several important respects. First, the eclipses are shallow, V-shaped dips, suggesting that the inclination angle is relatively low. Also, while the excitation of the emission lines are r elatively high (He II comparable to H-beta), they are relatively weak compared to the continuum. The high Balmer lines have broad absorption wings, characteristic of an optically thick accretion disk. Yet there is evidence for a ''hot spot'' in the system, which reaches peak brig htness near phase 0.9 before the eclipse. Perhaps the most puzzling pr operty of this system is that the H-alpha emission line radial velocit y leads rather than lags the expected position for the location of the accretion disk. We present briefly a phenomenological model for the s ystem which has a hot spot located at the normal location for the accr etion stream to first impact the disk and is the source of excess opti cal continuum. However, the velocity curve of the emission lines requi res us to conclude that the bulk of this radiation forms on the opposi te side of the disk. This also explains the fact that the peak equival ent widths of H-alpha occur at phases 0.4-0.5.