We study the effects of a reduced mass-loss rate on the evolution of low metallicity Jsolated stars , following our earlier classification for angular momentum ( J ) isolated stars .
By using the stellar evolution code MESA we study the evolution with different mass-loss rate efficiencies for stars with low metallicities of Z = 0.001 and Z = 0.004 , and compare with the evolution with solar metallicity , Z = 0.02 .
We further study the possibility for late asymptomatic giant branch ( AGB ) —planet interaction and its possible effects on the properties of the planetary nebula ( PN ) .
We find for all metallicities that only with a reduced mass-loss rate an interaction with a low mass companion might take place during the AGB phase of the star .
The interaction will most likely shape an elliptical PN .
The maximum post-AGB luminosities obtained , both for solar metallicity and low metallicities , reach high values corresponding to the enigmatic finding of the PN luminosity function .