  The old nova V728 Sco has been recently recovered via photometric and
spectroscopic observations, 150 years after the nova eruption. The spectral
properties pointed to a high-inclination system with a comparatively low
mass-transfer rate. In this paper we show that the object is an eclipsing
system with an orbital period of 3.32 h. It has enhanced long-term variability
that can be interpreted as 'stunted' dwarf-nova-type outbursts. Using the
ingress and egress times of the eclipsed components we calculate the radius of
the central object. The latter turns out to be significantly larger than a
white dwarf and we identify it with a hot inner disc. The implications for
models on the behaviour of post-novae are discussed.
