  We obtained photometric observations of the nova-like cataclysmic variable RW
Tri and gathered all available AAVSO and other data from the literature. We
determined the system parameters and found their uncertainties using the code
developed by us to model the light curves of binary systems. New time-resolved
optical spectroscopic observations of RW Tri were also obtained to study the
properties of emission features produced by the system. The usual
interpretation of the single-peaked emission lines in nova-like systems is
related to the bi-conical wind from the accretion disc's inner part. However,
we found that the Halpha emission profile is comprised of two components with
different widths. We argue that the narrow component originates from the
irradiated surface of the secondary, while the broader component's source is an
extended, low-velocity region in the outskirts of the accretion disc, located
opposite to the collision point of the accretion stream and the disc. It
appears to be a common feature for long-period nova-like systems -- a point we
discuss.
