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A classical nova is an eruption on the surface of a white dwarf in anaccreting binary system. The material ejected from the white dwarf surfacegenerally forms an axisymmetric shell. The shaping mechanisms of nova shellsare probes of the processes that take place at energy scales between planetarynebulae and supernova remnants. We report on the discovery of nova shellssurrounding the post-nova systems V4362 Sagittarii (1994) and more limitedobservations of DO Aquilae (1925). Distance measurements of 0.5p/m1.4 kpc forV4362 Sgr and 6.7 p/m 3.5 kpc -0.2 for DO Aql are found based on the expansionparallax method. The growth rates are measured to be 0.07``/year for DO Aql and0.32``/year for V4362 Sgr. A preliminary investigation into the ionisationstructure of the nova shell associated with V4362 Sgr is presented. Theobserved ionisation structure of nova shells depends strongly on theirmorphology and the orientation of the central component towards the observer.X-ray, IR and UV observations as well as optical integral field unitspectroscopy are required to better understand these interesting objects.

Two New Nova Shells associated with V4362 Sagittarii and DO Aquilae