  On the basis of spectrophotometric observations we reconstruct the accretion
disk of the eclipsing novalike cataclysmic variable RW Tri in the wavelength
region 3600-7000 A. We find a radial temperature profile that is, on average,
consistent with that expected on the basis of the theory of optically thick,
steady state accretion disks and infer a mass-accretion rate in RW Tri of
\~10e-8 solar masses per year. The line emission is dominated by two areas: one
around the hot-spot region and one near the white dwarf. Both emission regions
have appreciable vertical extension, and seem to be decoupled from the velocity
field in the disk. In our observations RW Tri shows a number of features that
are characteristic of the SW Sex sub-class of novalike stars. The appearance of
a novalike system as a UX UMa/RW Tri or SW Sex star seems to be mainly governed
by the mass-transfer rate from the secondary at the time of observation.
