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Title: Mass ejection in failed supernovae: variation with stellar progenitor

Abstract

We study the ejection of mass during stellar core-collapse when the stalled shock does not revive and a black hole forms. Neutrino emission during the protoneutron star phase causes a decrease in the gravitational mass of the core, resulting in an outward going sound pulse that steepens into a shock as it travels out through the star. We explore the properties of this mass ejection mechanism over a range of stellar progenitors using spherically symmetric, time-dependent hydrodynamic simulations that treat neutrino mass-loss parametrically and follow the shock propagation over the entire star. We find that all types of stellar progenitor can eject mass through this mechanism. The ejected mass is a decreasing function of the surface gravity of the star, ranging from several M for red supergiants to ~0.1 M for blue supergiants and ~10 -3 M for Wolf–Rayet stars. We find that the final shock energy at the surface is a decreasing function of the core-compactness, and is ≲ 10 47–10 48 erg in all cases. In progenitors with a sufficiently large envelope, high core-compactness, or a combination of both, the sound pulse fails to unbind mass. Successful mass ejection is accompanied by significant fallback accretionmore » that can last from hours to years. We predict the properties of shock breakout and thermal plateau emission produced by the ejection of the outer envelope of blue supergiant and Wolf–Rayet progenitors in otherwise failed supernovae.« less

Authors:
 [1];  [2];  [3];  [2]
  1. Univ. of Alberta, Edmonton, AB (Canada)
  2. Univ. of California, Berkeley, CA (United States)
  3. Univ. of Tokyo (Japan)
Publication Date:
Research Org.:
Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC); Univ. of California, Oakland, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1543976
Grant/Contract Number:  
AC02-05CH11231
Resource Type:
Accepted Manuscript
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Volume: 476; Journal Issue: 2; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Astronomy & Astrophysics

Citation Formats

Fernández, Rodrigo, Quataert, Eliot, Kashiyama, Kazumi, and Coughlin, Eric R. Mass ejection in failed supernovae: variation with stellar progenitor. United States: N. p., 2018. Web. doi:10.1093/mnras/sty306.
Fernández, Rodrigo, Quataert, Eliot, Kashiyama, Kazumi, & Coughlin, Eric R. Mass ejection in failed supernovae: variation with stellar progenitor. United States. doi:10.1093/mnras/sty306.
Fernández, Rodrigo, Quataert, Eliot, Kashiyama, Kazumi, and Coughlin, Eric R. Fri . "Mass ejection in failed supernovae: variation with stellar progenitor". United States. doi:10.1093/mnras/sty306. https://www.osti.gov/servlets/purl/1543976.
@article{osti_1543976,
title = {Mass ejection in failed supernovae: variation with stellar progenitor},
author = {Fernández, Rodrigo and Quataert, Eliot and Kashiyama, Kazumi and Coughlin, Eric R.},
abstractNote = {We study the ejection of mass during stellar core-collapse when the stalled shock does not revive and a black hole forms. Neutrino emission during the protoneutron star phase causes a decrease in the gravitational mass of the core, resulting in an outward going sound pulse that steepens into a shock as it travels out through the star. We explore the properties of this mass ejection mechanism over a range of stellar progenitors using spherically symmetric, time-dependent hydrodynamic simulations that treat neutrino mass-loss parametrically and follow the shock propagation over the entire star. We find that all types of stellar progenitor can eject mass through this mechanism. The ejected mass is a decreasing function of the surface gravity of the star, ranging from several M⊙ for red supergiants to ~0.1 M⊙ for blue supergiants and ~10-3 M⊙ for Wolf–Rayet stars. We find that the final shock energy at the surface is a decreasing function of the core-compactness, and is ≲ 1047–1048 erg in all cases. In progenitors with a sufficiently large envelope, high core-compactness, or a combination of both, the sound pulse fails to unbind mass. Successful mass ejection is accompanied by significant fallback accretion that can last from hours to years. We predict the properties of shock breakout and thermal plateau emission produced by the ejection of the outer envelope of blue supergiant and Wolf–Rayet progenitors in otherwise failed supernovae.},
doi = {10.1093/mnras/sty306},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 2,
volume = 476,
place = {United States},
year = {2018},
month = {2}
}

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