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How massive stars end their lives depends on the core mass, core angularmomentum, and hydrogen envelopes at death. However, these key physical facetsof stellar evolution can be severely affected by binary interactions. In turn,the effectiveness of binary interactions itself varies greatly depending on theinitial conditions of the binaries, making the situation much more complex. Weinvestigate systematically how binary interactions influence core-collapseprogenitors and their fates. Binary evolution simulations are performed tosurvey the parameter space of supernova progenitors in solar metallicity binarysystems and to delineate major evolutionary paths. We first study fixed binarymass ratios ($q=M_2/M_1$ = 0.5, 0.7, and 0.9) to elucidate the impacts ofinitial mass and initial separation on the outcomes, treating separately TypeIbc supernova, Type II supernova, accretion induced collapse (AIC), rapidlyrotating supernova (RSN), black hole formation, and gamma ray burst (GRB). Wethen conduct Binary Population Synthesis calculations for 12 models, varyingthe initial parameter distributions and binary evolution parameters, toestimate various supernova fractions. We obtain a Milky Way supernova rate$R_{\rm SN} = (1.14$--$1.57) \times10^{-2} \, {\rm yr}^{-1}$ which isconsistent with observations. We find the rates of AIC, RSN, and GRB to be$\sim 1/100$ the rate of regular supernovae. Our estimated GRB rates are higherthan the observed long GRB rate, but very close to the low luminosity GRB rate.Furthering binary modeling and improving the inputs one by one will enable moredetailed studies of these and other transients associated with massive stars.

Fate of supernova progenitors in massive binary systems