Evolution of low mass population III stars from the pre-main sequence to the white dwarf cooling track

Radiation feedback from massive population III stars may have given rise to low mass star formation from primordial or nearly primordial material. If early Universe low mass stars did form, some should remain locally as white dwarfs, sub-giants, or main sequence stars. In this paper, we present model calculations for the evolution of single 0.8-3.0 M⊙ stars with primordial metallicity from pre-main sequence to the white dwarf cooling track, and calculations for the evolution of single 4.0-7.0 M⊙ stars which conclude in the giant phase. One goal of this work is to identify potential observable markers for potential observed progenitors of first or nearly first stars. We uncover a number of seemingly peculiar evolutionary differences between that of population III low mass stars compared with younger higher Z stars, as well as compared to other primordial evolution models. We also present an initial-final mass relationship and identify the minimum mass of a single white dwarf that could have had a population III progenitor.

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2023 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

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Work Title Evolution of low mass population III stars from the pre-main sequence to the white dwarf cooling track
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Open Access
Creators
  1. T. M. Lawlor
  2. J. Macdonald
Keyword
  1. Stars: abundances
  2. Stars: AGB and post-AGB
  3. Stars: evolution
  4. Stars: Population III
  5. White dwarfs
License In Copyright (Rights Reserved)
Work Type Article
Publisher
  1. Monthly Notices of the Royal Astronomical Society
Publication Date September 2, 2023
Publisher Identifier (DOI)
  1. https://doi.org/10.1093/mnras/stad2582
Deposited February 03, 2024

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  • Created

    February 03, 2024 10:58 by Researcher Metadata Database

  • Added stad2582_1_-1.pdf

    February 03, 2024 10:58 by Researcher Metadata Database

  • Added Creator T. M. Lawlor

    February 03, 2024 10:58 by Researcher Metadata Database

  • Added Creator J. Macdonald

    February 03, 2024 10:58 by Researcher Metadata Database

  • Published

    February 03, 2024 10:58 by Researcher Metadata Database

  • Updated Keyword, Description Show Changes

    February 05, 2024 15:33 by avs5190

    Keyword
    • Stars: abundances, Stars: AGB and post-AGB, Stars: evolution, Stars: Population III, White dwarfs
    Description
    • Radiation feedback from massive population III stars may have given rise to low mass star formation from primordial or nearly primordial material. If early Universe low mass stars did form, some should remain locally as white dwarfs, sub-giants, or main sequence stars. In this paper, we present model calculations for the evolution of single 0.8-3.0 M stars with primordial metallicity from pre-main sequence to the white dwarf cooling track, and calculations for the evolution of single 4.0-7.0 M stars which conclude in the giant phase. One goal of this work is to identify potential observable markers for potential observed progenitors of first or nearly first stars. We uncover a number of seemingly peculiar evolutionary differences between that of population III low mass stars compared with younger higher Z stars, as well as compared to other primordial evolution models. We also present an initial-final mass relationship and identify the minimum mass of a single white dwarf that could have had a population III progenitor.
    • Radiation feedback from massive population III stars may have given rise to low mass star formation from primordial or nearly primordial material. If early Universe low mass stars did form, some should remain locally as white dwarfs, sub-giants, or main sequence stars. In this paper, we present model calculations for the evolution of single 0.8-3.0 M⊙ stars with primordial metallicity from pre-main sequence to the white dwarf cooling track, and calculations for the evolution of single 4.0-7.0 M⊙ stars which conclude in the giant phase. One goal of this work is to identify potential observable markers for potential observed progenitors of first or nearly first stars. We uncover a number of seemingly peculiar evolutionary differences between that of population III low mass stars compared with younger higher Z stars, as well as compared to other primordial evolution models. We also present an initial-final mass relationship and identify the minimum mass of a single white dwarf that could have had a population III progenitor.
  • Updated

    April 04, 2024 10:22 by [unknown user]