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Recent interpretations of narrow, variable absorption lines detected in someType Ia supernovae suggest that their progenitors are surrounded by dense,circumstellar material. Similar variations detected in the symbiotic recurrentnova system RS Oph, which undergoes thermonuclear outbursts every ~20 years,making it an ideal candidate to investigate the origin of these lines. To thisend, we present simulations of multiple mass transfer-nova cycles in RS Oph. Wefind that the quiescent mass transfer produces a dense, equatorial outflow,i.e., concentrated towards the binary orbital plane, and an accretion discforms around the white dwarf. The interaction of a spherical nova outburst withthese aspherical circumstellar structures produces a bipolar outflow, similarto that seen in HST imaging of the 2006 outburst. In order to produce anionization structure that is consistent with observations, a mass-loss rate of$5 \times 10^{-7}\,\mathrm{M}_{\odot}\,\mathrm{yr}^{-1}$ from the red giant isrequired. The simulations also produce a polar accretion flow, which mayexplain the broad wings of the quiescent H {\alpha} line and hard X-rays. Bycomparing simulated absorption line profiles to observations of the 2006outburst, we are able to determine which components arise in the wind and whichare due to the novae. We explore the possible behaviour of absorption lineprofiles as they may appear should a supernova occur in a system like RS Oph.Our models show similarities to supernovae like SN 2006X, but require a highmass-loss rate, $\dot{M} \sim 10^{-6}$ to$10^{-5}\,\mathrm{M_\odot}\,\mathrm{yr}^{-1}$, to explain the variability in SN2006X.

Modelling the circumstellar medium in RS Ophiuchi and its link to Type Ia supernovae