F. R. N. Schneider, E. Laplace, Ph. Podsiadlowski

As most massive stars are born in binary and other multiple-star systems, many are expected to exchange mass with a companion star or merge with it during their lives. This means that most supernovae (SNe) are from such binary products. Here, we focus on hydrogen-rich Type II SNe from accretors of binary mass transfer and stellar mergers. We compute various SN properties such as the explosion energies, nickel yields, and neutron star (NS) kick velocities, but also consider NS masses. We find tight correlations between these parameters and, e.g., the central specific entropy and core compactness. However, there is no obvious relation between these explosion properties and the evolutionary history of the pre-SN stars. We find linear relations between the nickel mass and the SN explosion energy and the NS remnant mass. We further group our models into progenitors of SNe IIP, SN 1987A-like and interacting SNe, predict their SN and SN-progenitor properties and compare to observations. Accretors of binary mass transfer and stellar mergers naturally produce SNe IIP with long plateau durations from progenitors with relatively small CO-cores but large envelope masses (c.f. SN 2015ba). Our models give rise to tight relations between the plateau luminosity and the nickel mass as well as the SN ejecta velocity as inferred observationally for SNe IIP. We speculate that cool/red supergiants at $\log\,L/L_\odot\,{\geq}\,5.5$ encounter enhanced mass loss due to envelope instabilities and could then explode in interacting SNe IIn. The rate of such SNe from our models seems compatible with observations. Some of our binary models explode as $10^6\,L_\odot$ blue supergiants that may have encountered enhanced and/or eruptive mass loss shortly before their SNe and could thus help understand interacting SNe such as SN 1961V and SN 2005gl but also superluminous Type II SNe such as SN 2010jl. [abridged]