We argue that all transient searches for planets in globular clusters are hopeless. Planets in low metallicity stars typically don't reside at small orbital separations. The dependance of planetary system properties on metallicity is clearly seen when the quantity of the planet mass times periastron distance square (Ie) is considered. 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 (in units of Jupiter mass times AU square). In low metallicity systems the concentration is only at the higher range of Ie. Therefore, it is still possible that planets exist around main sequence stars in globular clusters, although very rarely because of the low metallicity, but at orbital periods of >10 day. 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.