On the role of reduced wind mass-loss rate in enabling exoplanets to
  shape planetary nebulae
  We use the stellar evolution code MESA-binary and follow the evolution of
three exoplanets and two brown dwarfs (BDs) to determine their potential role
in the future evolution of their parent star on the red giant branch (RGB) and
on the asymptotic giant branch (AGB). We limit this study to exoplanets and BDs
with orbits that have semi-major axis of 1AU<a0<20AU, a high eccentricity,
e0>0.25, and having a parent star of mass M>1Mo. We find that the star HIP
75458 will engulf its planet HIP 75458 b during its RGB phase. The planet will
remove the envelope and terminate the RGB evolution, leaving a bare helium core
of mass 0.4Mo that will evolve to form a helium white dwarf. Only in one system
out of five, the planet beta Pic c will enter the envelope of its parent star
during the AGB phase. For that to occur, we have to reduce the wind mass-loss
rate by a factor of about four from its commonly used value. This strengthens
an early conclusion, which was based on exoplanets with circular orbits, that
states that to have a non-negligible fraction of AGB stars that engulf planets
we should consider lower wind mass-loss rates of isolated AGB stars (before
they are spun-up by a companion). Such an engulfed planet might lead to the
shaping of the AGB mass-loss geometry to form an elliptical planetary nebula.
