We evolve stellar models to study the common envelope (CE) interaction of an
early asymptotic giant branch star of initial mass 5Mââ with a
companion star of mass ranging from 0.1 to 2Mââ. We model the
CE as a fast stripping phase in which the primary experiences rapid mass loss
and loses about 80 per cent of its mass. The post-CE remnant is then allowed to
thermally readjust during a Roche-lobe overflow (RLOF) phase and the final
binary system and its orbital period are investigated. We find that the post-CE
RLOF phase is long enough to allow nuclear burning to proceed in the helium
shell. By the end of this phase, the donor is stripped of both its hydrogen and
helium and ends up as carbon-oxygen white dwarf of mass about 0.8Mââ. We study the sensitivity of our results to initial conditions of
different companion masses and orbital separations at which the stripping phase
begins. We find that the companion mass affects the final binary separation and
that helium-shell burning causes the star to refill its Roche lobe leading to
post-CE RLOF. Our results show that double mass transfer in such a binary
interaction is able to strip the helium and hydrogen layers from the donor star
without the need for any special conditions or fine tuning of the binary
parameters