Two New Nova Shells associated with V4362 Sagittarii and DO Aquilae

TL;DR

This paper reports the discovery and analysis of nova shells around V4362 Sagittarii and DO Aquilae, providing insights into their structure, expansion, and ionisation, which inform models of nova shell shaping mechanisms.

Contribution

It presents the first observations of nova shells around these systems, measures their distances, growth rates, and explores their ionisation structures, advancing understanding of nova shell morphology.

Findings

Discovered nova shells around V4362 Sgr and DO Aql.

Measured expansion rates of 0.07''/year and 0.32''/year.

Estimated distances of approximately 0.5 and 6.7 kpc.

Abstract

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.