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Galaxies 2018, 6(3), 89;

Jsolated Stars of Low Metallicity

Department of Physics, Technion—Israel Institute of Technology, Haifa 32000, Israel
Received: 15 July 2018 / Revised: 8 August 2018 / Accepted: 9 August 2018 / Published: 15 August 2018
(This article belongs to the Special Issue Asymmetric Planetary Nebulae VII)
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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. View Full-Text
Keywords: late stage stellar evolution; planetary nebulae; binarity; stellar evolution late stage stellar evolution; planetary nebulae; binarity; stellar evolution

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Sabach, E. Jsolated Stars of Low Metallicity. Galaxies 2018, 6, 89.

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