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Title: Effects of axions on Population III stars

Abstract

Following the renewed interest in axions as a dark matter component, we revisit the effects of energy loss by axion emission on the evolution of the first generation of stars. These stars with zero metallicity are assumed to be massive, more compact, and hotter than subsequent generations. It is hence important to extend previous studies, which were restricted to solar metallicity stars. Here, our analysis first compares the evolution of solar metallicity 8, 10, and 12 M stars to previous work. We then calculate the evolution of 8 zero-metallicity stars with and without axion losses and with masses ranging from 20 to 150 M . For the solar metallicity models, we confirm the disappearance of the blue-loop phase for a value of the axion-photon coupling of g = 10 -10 GeV -1. We show that for g = 10 -10 GeV -1, the evolution of Population III stars is not much affected by axion losses, except within the range of masses 80–130 M . Such stars show significant differences in both their tracks within the Tc–ρc diagram and their central composition (in particular 20Ne and 24Mg). We discuss the origin of these modifications from the stellar physics point ofmore » view, and also their potential observational signatures.« less

Authors:
 [1];  [2];  [1];  [3];  [4];  [5]
  1. Univ. of Geneva, Sauverny (Switzerland). Geneva Observatory
  2. Univ. Paris-Saclay, Orsay (France). Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM)
  3. Univ. of Minnesota, Minneapolis, MN (United States). School of Physics and Astronomy, William I. Fine Theoretical Physics Inst.
  4. Univ. Pierre et Marie Curie, Paris (France). Inst. d'Astrophysique de Paris; Sorbonne Univ., Paris (France). Inst. Lagrange de Paris
  5. Univ. Pierre et Marie Curie, Paris (France). Inst. d'Astrophysique de Paris; Sorbonne Univ., Paris (France). Inst. Lagrange de Paris
Publication Date:
Research Org.:
Univ. of Minnesota, Minneapolis, MN (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1535275
Grant/Contract Number:  
SC0011842
Resource Type:
Accepted Manuscript
Journal Name:
Astronomy and Astrophysics
Additional Journal Information:
Journal Volume: 605; Journal ID: ISSN 0004-6361
Publisher:
EDP Sciences
Country of Publication:
United States
Language:
English
Subject:
astronomy & astrophysics; elementary particles; star evolution; Population III; massive stars

Citation Formats

Choplin, Arthur, Coc, Alain, Meynet, Georges, Olive, Keith A., Uzan, Jean-Philippe, and Vangioni, Elisabeth. Effects of axions on Population III stars. United States: N. p., 2017. Web. doi:10.1051/0004-6361/201731040.
Choplin, Arthur, Coc, Alain, Meynet, Georges, Olive, Keith A., Uzan, Jean-Philippe, & Vangioni, Elisabeth. Effects of axions on Population III stars. United States. doi:10.1051/0004-6361/201731040.
Choplin, Arthur, Coc, Alain, Meynet, Georges, Olive, Keith A., Uzan, Jean-Philippe, and Vangioni, Elisabeth. Mon . "Effects of axions on Population III stars". United States. doi:10.1051/0004-6361/201731040. https://www.osti.gov/servlets/purl/1535275.
@article{osti_1535275,
title = {Effects of axions on Population III stars},
author = {Choplin, Arthur and Coc, Alain and Meynet, Georges and Olive, Keith A. and Uzan, Jean-Philippe and Vangioni, Elisabeth},
abstractNote = {Following the renewed interest in axions as a dark matter component, we revisit the effects of energy loss by axion emission on the evolution of the first generation of stars. These stars with zero metallicity are assumed to be massive, more compact, and hotter than subsequent generations. It is hence important to extend previous studies, which were restricted to solar metallicity stars. Here, our analysis first compares the evolution of solar metallicity 8, 10, and 12 M⊙ stars to previous work. We then calculate the evolution of 8 zero-metallicity stars with and without axion losses and with masses ranging from 20 to 150 M⊙. For the solar metallicity models, we confirm the disappearance of the blue-loop phase for a value of the axion-photon coupling of gaγ = 10-10 GeV-1. We show that for gaγ = 10-10 GeV-1, the evolution of Population III stars is not much affected by axion losses, except within the range of masses 80–130 M⊙. Such stars show significant differences in both their tracks within the Tc–ρc diagram and their central composition (in particular 20Ne and 24Mg). We discuss the origin of these modifications from the stellar physics point of view, and also their potential observational signatures.},
doi = {10.1051/0004-6361/201731040},
journal = {Astronomy and Astrophysics},
number = ,
volume = 605,
place = {United States},
year = {2017},
month = {9}
}

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