RS Oph at day 201: a test case for shocks in nova shells

Open Access
Publisher Website
Google Scholar
Abstract
We have applied a shock model to the nebula ejected in 1985 by the recurrent nova RS Oph. The model, based on the SUMA code, matches the relative line intensities observed at day 201 after outburst and yields element abundances relative to hydrogen, density and temperature profiles throughout the shocked region, and integrated fluxes in all ranges of the spectrum. We have investigated the effect of dust and the contribution of a hot star as an additional photoionization source. We find that the entire spectrum is well explained by shocks, even neglecting any other photoionizing source. In particular, the residual X-ray emission detected more than 200 d after outburst can be the result of shocks. The estimated distance of the shock front from the central star is of the order of 5 × 1015 cm. The high helium abundance, as well as the very low oxygen abundance resulting from this model, is shown to agree with the thermonuclear runaway scenario for recurrent novae, which involves accretion on to a very massive white dwarf.

This publication has 0 references indexed in Scilit: