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

Understand

Neutron-star (NS) - white-dwarf (WD) mergers may give rise to observable explosive transients, but have been little explored.

• We use 2D coupled hydrodynamical-thermonuclear FLASH-code simulations to study the evolution of WD debris-disks formed following WD-disruptions by NSs.
• We use a 19-elements nuclear-network and a detailed equation-of-state to follow the evolution, complemented by a post-process analysis using a larger 125-isotopes nuclear-network.
• We consider a wide range of initial conditions and study the dependence of the results on the NS/WD masses ($1.4-2{\rm M_{\odot}}$;$\,{\rm 0.375-0.7\,M_{\odot}}$, respectively), WD-composition (CO/He/hybrid-He-CO) and the accretion-disk structure.