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Title: A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations

Abstract

ABSTRACT This paper presents the first systematic study of proto-neutron star (PNS) convection in three dimensions (3D) based on our latest numerical fornax models of core-collapse supernova (CCSN). We confirm that PNS convection commonly occurs, and then quantify the basic physical characteristics of the convection. By virtue of the large number of long-term models, the diversity of PNS convective behaviour emerges. We find that the vigour of PNS convection is not correlated with CCSN dynamics at large radii, but rather with the mass of PNS − heavier masses are associated with stronger PNS convection. We find that PNS convection boosts the luminosities of νμ, ντ, $$\bar{\nu }_{\mu }$$, and $$\bar{\nu }_{\tau }$$ neutrinos, while the impact on other species is complex due to a competition of factors. Finally, we assess the consequent impact on CCSN dynamics and the potential for PNS convection to generate pulsar magnetic fields.

Authors:
 [1];  [1]; ORCiD logo [2];  [3]
  1. Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USA
  2. Department of Physics, The Pennsylvania State University, University Park, PA 16802, USA, Department of Astronomy & Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA
  3. Astronomy Department and Theoretical Astrophysics Center, University of California, Berkeley, CA 94720, USA
Publication Date:
Sponsoring Org.:
USDOE
OSTI Identifier:
1598917
Grant/Contract Number:  
SC0018297; AC02-06CH11357; AC03-76SF00098
Resource Type:
Published Article
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 492 Journal Issue: 4; Journal ID: ISSN 0035-8711
Publisher:
Oxford University Press
Country of Publication:
United Kingdom
Language:
English

Citation Formats

Nagakura, Hiroki, Burrows, Adam, Radice, David, and Vartanyan, David. A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations. United Kingdom: N. p., 2020. Web. doi:10.1093/mnras/staa261.
Nagakura, Hiroki, Burrows, Adam, Radice, David, & Vartanyan, David. A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations. United Kingdom. doi:10.1093/mnras/staa261.
Nagakura, Hiroki, Burrows, Adam, Radice, David, and Vartanyan, David. Tue . "A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations". United Kingdom. doi:10.1093/mnras/staa261.
@article{osti_1598917,
title = {A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations},
author = {Nagakura, Hiroki and Burrows, Adam and Radice, David and Vartanyan, David},
abstractNote = {ABSTRACT This paper presents the first systematic study of proto-neutron star (PNS) convection in three dimensions (3D) based on our latest numerical fornax models of core-collapse supernova (CCSN). We confirm that PNS convection commonly occurs, and then quantify the basic physical characteristics of the convection. By virtue of the large number of long-term models, the diversity of PNS convective behaviour emerges. We find that the vigour of PNS convection is not correlated with CCSN dynamics at large radii, but rather with the mass of PNS − heavier masses are associated with stronger PNS convection. We find that PNS convection boosts the luminosities of νμ, ντ, $\bar{\nu }_{\mu }$, and $\bar{\nu }_{\tau }$ neutrinos, while the impact on other species is complex due to a competition of factors. Finally, we assess the consequent impact on CCSN dynamics and the potential for PNS convection to generate pulsar magnetic fields.},
doi = {10.1093/mnras/staa261},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 4,
volume = 492,
place = {United Kingdom},
year = {2020},
month = {1}
}

Journal Article:
Free Publicly Available Full Text
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DOI: 10.1093/mnras/staa261

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