  Energetic outflows from main sequence stars accreting mass at very high rates
might account for the powering of some eruptive objects, such as merging main
sequence stars, major eruptions of luminous blue variables, e.g., the Great
Eruption of Eta Carinae, and other intermediate luminosity optical transients
(ILOTs; Red Novae; Red Transients). These powerful outflows could potentially
also supply the extra energy required in the common envelope process and in the
grazing envelope evolution of binary systems. We propose that a massive
outflow/jets mediated by magnetic fields might remove energy and angular
momentum from the accretion disk to allow such high accretion rate flows. By
examining the possible activity of the magnetic fields of accretion disks we
conclude that indeed main sequence stars might accrete mass at very high rates,
up to ~0.01 Mo/yr for solar type stars, and up to ~1 Mo/yr for very massive
stars. We speculate that magnetic fields amplified in such extreme conditions
might lead to the formation of massive bipolar outflows that can remove most of
the disk's energy and angular momentum. It is this energy and angular momentum
removal that allows the very high mass accretion rate on to main sequence
stars.
