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We perform 3D hydrodynamical simulations of new-born neutron stars (NSs)colliding with main-sequence binary companions after supernova explosions.Based on those hydrodynamical models, we construct a semi-analytical formulathat describes the drag force inside stars with steep density gradients. Wethen compute the outcome of NS--companion collisions over a wide range ofparameters using the semi-analytical formula. Depending on the direction andmagnitude of the natal kick, we find that the collision may lead to variousoutcomes. For relatively fast kicks and high impact parameters, the NS maypenetrate the companion star envelope without merging. By allowing the NS toplunge through companions, the companion can be accelerated to have runawayvelocities up to $\sim10$ per cent above the theoretical upper limit consideredin classical binary disruption scenarios. The NS can capture and carry away upto a few per cent of the companion envelope as it escapes, which may formpulsar planets or cause outflows through accretion to heat the ejecta frominside and power the supernova light curve. For lower impact parameters, theneutron star will directly merge with the companion and form a Thorne-\.Zytkowobject. In intermediate cases, the NS penetrates the companion envelope severaltimes before merging, possibly causing multiple bumps in the supernova lightcurve like in SN2015bn and SN2019stc.

monthly notices of the royal astronomical society

Neutron stars colliding with binary companions: formation of  hypervelocity stars, pulsar planets, bumpy superluminous supernovae and  Thorne-\.Zytkow objects