  I examine the implications of the recently found extrasolar planets on the
planet-induced axisymmetrical mass loss model for the formation of elliptical
planetary nebulae (PNs). This model, which was developed in several earlier
papers by the author and a few collaborators, attributes low departure from
spherical mass loss of upper asymptotic giant branch (AGB) stars to envelope
rotation which results from deposition of planet's orbital angular momentum. It
was predicted that about 50 percent of all sun-like stars have Jupiter-like
planets around them. In light of the new finding that only 5 percent of
sun-like stars do have such planets I revise this prediction. I now predict
that indeed about 50 percent of PNs progenitors do have close planets around
them, but the planets can have much lower masses, as low as 0.01 times
Jupiter's mass. To support this claim I follow the angular momentum evolution
of single stars as they evolve to the post-AGB phase. The prediction that on
average several such planets orbit each star, as in the solar system, still
holds.
