  We propose a speculative scenario where dynamo amplification of magnetic
fields in the core convective shells of massive stars, tens of years to hours
before they explode, leads to envelope expansion and enhanced mass loss rate,
resulting in pre-explosion outbursts (PEOs). The convective luminosity in the
burning shells of carbon, neon, oxygen, and then silicon, are very high. Based
on the behavior of active main sequence stars we speculate that the convective
shells can trigger magnetic activity with a power of about 0.001 times the
convective luminosity. Magnetic flux tubes might buoy outward, and deposit
their energy in the outer parts of the envelope. This in turn might lead to the
expansion of the envelope and to an enhanced mass loss rate. If a close binary
companion is present, mass transfer might take place and lead to an energetic
outburst. The magnetic activity requires minimum core rotation and that the
stochastic magnetic activity be on its high phase. Only in rare cases these
conditions are met, accounting for that only the minority of core collapse
supernovae (CCSNe) experience PEO. Such a pre-explosion magnetic activity might
have implications for the explosion mechanism itself.
