  I consider three processes which enhance mass loss rate from a common
envelope of a giant star with a main sequence or a white dwarf companion
spiraling-in inside its envelope. I consider deposition of orbital energy and
orbital angular momentum to the giant's envelope, and in more detail the
formation of jets by an accreting companion and their propagation in the
envelope. I find that in many cases the deposition of orbital angular momentum
to the envelope may be more important to the mass loss process than the
deposition of orbital energy. Jets blown by an accreting companion, in
particular a white dwarf, orbiting inside the outer regions of the giant's
envelope may also dominate over orbital energy deposition at early stage of the
common envelope evolution. These imply that studies which ignore the deposition
of angular momentum to the envelope and the effects of the accreting companion
may reach wrong conclusions.
