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Context. Classical novae are thermonuclear explosions hosted by accretingwhite dwarfs in stellar binary systems. Material piles up on top of the whitedwarf star under mildly degenerate conditions, driving a thermonuclear runaway.The energy released by the suite of nuclear processes operating at the envelope(mostly proton-capture reactions and beta-decays) heats the material up to peaktemperatures ranging from 100 to 400 MK. In these events, about 10-3 - 10-7Msun, enriched in CNO and, sometimes, other intermediate-mass elements (e.g.,Ne, Na, Mg, Al), are ejected into the interstellar medium.  Aims. To date, most of the efforts undertaken in the modeling of classicalnova outbursts have focused on the early stages of the explosion and ejection,ignoring the interaction of the ejecta, first with the accretion disk orbitingthe white dwarf, and ultimately with the secondary star.  Methods. A suite of three-dimensional, SPH simulations of the interactionbetween the nova ejecta, the accretion disk, and the stellar companion havebeen performed to fill this gap, aimed at testing the influence of thedifferent parameters (i.e., mass and velocity of the ejecta, mass and geometryof the accretion disk) on the dynamical and chemical properties of the system.  Results. We discuss the conditions that lead to the disruption of theaccretion disk and to mass loss from the binary system. In addition, we discussthe likelihood of chemical contamination of the stellar secondary induced bythe impact with the nova ejecta and its potential effect on the next novacycle.

Three-dimensional simulations of the interaction between the nova ejecta, the accretion disk, and the companion star