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Neutron-star (NS) - white-dwarf (WD) mergers may give rise to observableexplosive transients, but have been little explored. We use 2D coupledhydrodynamical-thermonuclear FLASH-code simulations to study the evolution ofWD debris-disks formed following WD-disruptions by NSs. We use a 19-elementsnuclear-network and a detailed equation-of-state to follow the evolution,complemented by a post-process analysis using a larger 125-isotopesnuclear-network. We consider a wide range of initial conditions and study thedependence of the results on the NS/WD masses ($1.4-2{\rm M_{\odot}}$;$\,{\rm0.375-0.7\,M_{\odot}}$, respectively), WD-composition (CO/He/hybrid-He-CO) andthe accretion-disk structure. We find that viscous inflow in the disk givesrise to continuous wind-outflow of mostly C/O material mixed withnuclear-burning products arising from a weak detonation occurring in theinner-region of the disk. We find that such transients are energetically weak($10^{48}-10^{49}$ergs) compared with thermonuclear-supernovae (SNe), and aredominated by the (gravitational) accretion-energy. Althoughthermonuclear-detonations occur robustly in all of our simulations (besides theHe-WD) they produce only little energy $(1-10\%$ of the kinetic energy) and$^{56}{\rm Ni}$ ejecta (few$\times10^{-4}-10^{-3}{\rm M_{\odot}})$, withoverall low ejecta masses of $\sim0.01-0.1{\rm M_{\odot}}$. Such explosions mayproduce rapidly-evolving transients, much shorter and fainter than regulartype-Ia SNe. The composition and demographics of such SNe appear to beinconsistent with those of Ca-rich type Ib SNe. Though they might be related tothe various classes of rapidly evolving SNe observed in recent years, they arelikely to be fainter than the typical ones, and may therefore give rise adifferent class of potentially observable transients.

Neutron star - white dwarf mergers: Early evolution, physical properties, and outcomes