  A classical nova is an eruption on the surface of a white dwarf in an
accreting binary system. The material ejected from the white dwarf surface
generally forms an axisymmetric shell. The shaping mechanisms of nova shells
are probes of the processes that take place at energy scales between planetary
nebulae and supernova remnants. We report on the discovery of nova shells
surrounding the post-nova systems V4362 Sagittarii (1994) and more limited
observations of DO Aquilae (1925). Distance measurements of 0.5p/m1.4 kpc for
V4362 Sgr and 6.7 p/m 3.5 kpc -0.2 for DO Aql are found based on the expansion
parallax method. The growth rates are measured to be 0.07``/year for DO Aql and
0.32``/year for V4362 Sgr. A preliminary investigation into the ionisation
structure of the nova shell associated with V4362 Sgr is presented. The
observed ionisation structure of nova shells depends strongly on their
morphology and the orientation of the central component towards the observer.
X-ray, IR and UV observations as well as optical integral field unit
spectroscopy are required to better understand these interesting objects.
