2022MNRAS.516.1846H

We simulate the response of a main sequence star to the explosion of a stripped-envelope (type Ib or Ic) core-collapse supernova (CCSN) when the main sequence star orbits the core at a distance of $10 \, \mathrm{R}_\odot$ or $20 \, \mathrm{R}_\odot$ at explosion. We use the stellar evolution code MESA to follow the response of main sequence stars of masses $3 \, \mathrm{M}_\odot$ and $7\, \mathrm{M}_\odot$ to energy deposition and mass removal. The collision of the CCSN ejecta with the main sequence star deposits energy and inflate the main sequence star. If the binary system stays bound after the CCSN explosion, the inflated main sequence star might engulf the newly born neutron star (NS). We assume that the NS accretes mass through an accretion disc and launches jets. The jets remove mass from the inflated main sequence star and collide with the CCSN ejecta. Although this scenario is rare, it adds up to other rare scenarios to further support the notion that many stripped envelope CCSNe are powered by late jets. The late jets can power these CCSNe-I for a long time and might power bumps in their light curve. The jets might also shape the inner ejecta to a bipolar morphology. Our results further support suggestions that there are several ways to feed an NS (or a black hole) to launch the late jets in superluminous supernovae.