Jsolated Stars of Low Metallicity

TL;DR

This study investigates how reduced mass-loss rates affect the evolution of low-metallicity Jsolated stars, revealing potential for planetary interactions and elliptical planetary nebula formation across different metallicities.

Contribution

It introduces the effects of reduced mass-loss rates on low-metallicity Jsolated stars and their potential for planetary interactions during the AGB phase.

Findings

Reduced mass-loss rates enable AGB-planet interactions.

Interactions likely produce elliptical planetary nebulae.

High post-AGB luminosities match observed planetary nebula luminosity functions.

Abstract

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.