  We argue that all transient searches for planets in globular clusters have a
very low detection probability. Planets of low metallicity stars typically do
not reside at small orbital separations. The dependance of planetary system
properties on metallicity is clearly seen when the quantity Ie=Mp[a(1-e)]^2 is
considered; Mp, a, e, are the planet mass, semi-major axis, and eccentricity,
respectively. In high metallicity systems there is a concentration of systems
at high and low values of Ie, with a low-populated gap near Ie~0.3 M_J AU^2,
where M_J is Jupiter's mass. In low metallicity systems the concentration is
only at the higher range of I_e, with a tail to low values of Ie. Therefore, it
is still possible that planets exist around main sequence stars in globular
clusters, although at small numbers because of the low metallicity, and at
orbital periods of >~10 days. We discuss the implications of our conclusions on
the role that companions can play in the evolution of their parent stars in
globular clusters, e.g., influencing the distribution of horizontal branch
stars on the Hertzsprung-Russell diagram of some globular clusters, and in
forming low mass white dwarfs.
