  We study the evolution of six exoplanetary systems with the stellar
evolutionary code MESA and conclude that they will likely spin-up the envelope
of their parent stars on the red giant branch (RGB) or later on the asymptotic
giant branch (AGB) to the degree that the mass loss process might become
non-spherical. We choose six observed exoplanetary systems where the semi-major
axis is ~1-2AU, and use the binary mode of MESA to follow the evolution of the
systems. In four systems the star engulfs the planet on the RGB, and in two
systems on the AGB, and the systems enter a common envelope evolution (CEE). In
two systems where the exoplanet masses are Mp~10MJ, where MJ is Jupiter mass,
the planet spins-up the envelope to about 10% of the break-up velocity. Such
envelopes are likely to have significant non-spherical mass loss geometry. In
the other four systems where Mp~MJ the planet spins-up the envelope to values
of ~1-2% of break-up velocity. Magnetic activity in the envelope that
influences dust formation might lead to a small departure from spherical mass
loss even in these cases. In the two cases of CEE on the AGB the planet
deposits energy to the envelope that amounts to >10% of the envelope binding
energy. We expect this to cause a non-spherical mass loss that will shape an
elliptical planetary nebula in each case.
