2024MNRAS.52710025C

We conduct one-dimensional stellar evolutionary numerical simulations under the assumption that an efficient dynamo operates in the core of massive stars years to months before core collapse and find that the magnetic activity enhances mass-loss rate and might trigger binary interaction that leads to outbursts. We assume that the magnetic flux tubes that the dynamo forms in the inner core buoy out to the outer core where there is a steep entropy rise and a molecular weight drop. There the magnetic fields turn to thermal energy, i.e. by reconnection. We simulate this energy deposition where the entropy steeply rises and find that for our simulated cases the envelope radius increases by a factor of ≃1.2-2 and luminosity by about an order of magnitude. These changes enhance the mass-loss rate. The envelope expansion can trigger a binary interaction that powers an outburst. Because magnetic field amplification depends positively on the core rotation rate and operates in cycles, not in all cases the magnetic activity will be powerful enough to change envelope properties. Namely, only a fraction of core-collapse supernovae experiences pre-explosion outbursts.