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:
-
[2];
- Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USA
- 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
- Astronomy Department and Theoretical Astrophysics Center, University of California, Berkeley, CA 94720, USA
- Publication Date:
- Research Org.:
- Univ. of California, Oakland, CA (United States); Argonne National Lab. (ANL), Argonne, IL (United States); Univ. of California, San Diego, CA (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC)
- OSTI Identifier:
- 1598917
- Alternate Identifier(s):
- OSTI ID: 1803352
- 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
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; Astronomy & Astrophysics
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. https://doi.org/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. https://doi.org/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}
}
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