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We obtained Hubble STIS spectra of three nova-like variables: V751 Cygni,V380 Oph, and - the only confirmed nova-like variable known to be below theperiod gap - BK Lyn. In all three systems, the spectra were taken during highoptical brightness state, and a luminous accretion disk dominates their farultraviolet (FUV) light. We assessed a lower limit of the distances by applyingthe infrared photometric method of \citet{Knigge2006}. Within the limitationsimposed by the poorly known system parameters (such as the inclination, whitedwarf mass, and the applicability of steady state accretion disks) we obtainedsatisfactory fits to BK Lyn using optically thick accretion disk models with anaccretion rate of $\dot{M} = 1\times10^{-9} M_{\odot}$ yr$^{-1}$ for a whitedwarf mass of $M_{wd} = 1.2 M_{\odot}$ and $\dot{M} = 1 \times 10^{-8}M_{\odot}$ yr$^{-1}$ for $M_{wd} = 0.4 M_{\odot}$. However, for the VY Scl-typenova-like variable V751 Cygni and for the SW Sex star V380 Oph, we are unableto obtain satisfactory synthetic spectral fits to the high state FUV spectrausing optically thick steady state accretion disk models. The lack of FUVspectra information down to the Lyman limit hinders the extraction ofinformation about the accreting white dwarf during the high states of thesenova-like systems.

Hubble Space Telescope STIS Spectroscopy of Three Peculiar Nova-Like Variables: BK Lyn, V751 Cygni and V380 Oph