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Neutrino-Driven Convection in Core-Collapse Supernovae: High-Resolution Simulations

Radice, David and Ott, Christian D. and Abdikamalov, Ernazar and Couch, Sean M. and Haas, Roland and Schnetter, Erik (2016) Neutrino-Driven Convection in Core-Collapse Supernovae: High-Resolution Simulations. Astrophysical Journal, 820 (1). Art. No. 76. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20160307-101746459

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Abstract

We present results from high-resolution semiglobal simulations of neutrino-driven convection in core-collapse supernovae. We employ an idealized setup with parametrized neutrino heating/cooling and nuclear dissociation at the shock front. We study the internal dynamics of neutrino-driven convection and its role in re-distributing energy and momentum through the gain region. We find that even if buoyant plumes are able to locally transfer heat up to the shock, convection is not able to create a net positive energy flux and overcome the downwards transport of energy from the accretion flow. Turbulent convection does, however, provide a significant effective pressure support to the accretion flow as it favors the accumulation of energy, mass and momentum in the gain region. We derive an approximate equation that is able to explain and predict the shock evolution in terms of integrals of quantities such as the turbulent pressure in the gain region or the effects of nonradial motion of the fluid. We use this relation as a way to quantify the role of turbulence in the dynamics of the accretion shock. Finally, we investigate the effects of grid resolution, which we change by a factor 20 between the lowest and highest resolution. Our results show that the shallow slopes of the turbulent kinetic energy spectra reported in previous studies are a numerical artefact. Kolmogorov scaling is progressively recovered as the resolution is increased.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1510.05022arXivDiscussion Paper
http://dx.doi.org/10.3847/0004-637X/820/1/76DOIArticle
http://iopscience.iop.org/article/10.3847/0004-637X/820/1/76/metaPublisherArticle
ORCID:
AuthorORCID
Radice, David0000-0001-6982-1008
Ott, Christian D.0000-0003-4993-2055
Haas, Roland0000-0003-1424-6178
Schnetter, Erik0000-0002-4518-9017
Additional Information:© 2016 The American Astronomical Society. Received 2015 October 16; accepted 2016 February 10; published 2016 March 21. We acknowledge helpful discussions with W. D. Arnett, A. Burrows, C. Meakin, P. Mösta, J. Murphy, and L. Roberts. This research was partially supported by the National Science Foundation under award nos. AST-1212170 and PHY-1151197 and by the Sherman Fairchild Foundation. The simulations were performed on the Caltech compute cluster Zwicky (NSF MRI-R2 award no. PHY-0960291), on the NSF XSEDE network under allocation TG-PHY100033, and on NSF/NCSA BlueWaters under NSF PRAC award no. ACI-1440083.
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
NSFAST-1212170
NSFPHY-1151197
Sherman Fairchild FoundationUNSPECIFIED
NSFPHY-0960291
NSFTG-PHY100033
NSFACI-1440083
Subject Keywords:hydrodynamics; supernovae: general; turbulence
Issue or Number:1
Record Number:CaltechAUTHORS:20160307-101746459
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20160307-101746459
Official Citation:David Radice et al 2016 ApJ 820 76
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:65108
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:09 Mar 2016 23:27
Last Modified:09 Mar 2020 13:19

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