Volume 33 number 1 (2005)
(Abstract only) From models for mass loss from pulsating Mira variables we know quite a bit about the conditions that planets will encounter when their stars reach the end of the AGB and the final mass loss epoch. I present some calculations and some speculations about the fates of planets like those in our solar system and discuss the conditions needed to detect the presence of planets at that stage of stellar evolution by photometric means.