Binary Interaction Dominates Mass Ejection in Classical Novae

Abstract Recent observations suggest our understanding of mass loss in classical novae is incomplete, motivating a new theoretical examination the physical processes responsible for nova ejection. In this paper, we perform hydrodynamical simulations outflows using stellar evolution code MESA . We find that, when binary companion neglected, white dwarfs with masses ≳0.8 M ⊙ successfully launch radiation-pressure-driven optically thick winds that carry away most envelope. However, mass-loss phase, these are accelerated at radii beyond dwarf’s Roche radius assuming typical cataclysmic variable donor. This means before standard wind can be formed, will instead initiated and shaped by interaction. An isotropic, only launched acceleration region recedes within radius, which occurs after envelope has already been ejected. The interaction between two modes outflow—a first phase slow, binary-driven, equatorially focused encompassing ejection second consisting fast, wind—is consistent aspherical ejecta signatures multiple outflow components. also isolated lower-mass ≲0.8 do not develop unbound any stage, making it even more crucial to consider effects on resulting outburst.