Mass loss and AGB evolution in Galactic satellites

Abstract

The effect of metallicity on the AGB mass loss is reviewed. Observations have mainly been limited to the Magellanic Clouds but are observationally feasible throughout the Local Group. Expansion velocities are predicted to depend strongly on Z but the peak mass-loss rates appear not to. The Mira PL relation shows no evidence for a Z-dependence, giving a powerful potential distance indicator: I derive a distance modulus to the LMC of$m-M = 18.63 +/- 0.09 as well as a bright calibration for the Horizontal Branch in globular clusters. Finally, the predicted initial-final mass relation at low Z is shown to give rise to higher mass remnants. This would result in an increased supernova rate in young, low-Z populations such as found in the early Universe.