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Neutrino-driven Convection in Core-collapse Supernovae: High-resolution Simulations

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dc.contributor.author Radice, David
dc.contributor.author Ott, Christian D.
dc.contributor.author Abdikamalov, Ernazar
dc.contributor.author Couch, Sean M.
dc.contributor.author Haas, Roland
dc.contributor.author Schnetter, Erik
dc.date.accessioned 2020-06-26T11:03:40Z
dc.date.available 2020-06-26T11:03:40Z
dc.date.issued 2016-03
dc.identifier.citation Radice, D., Ott, C. D., Abdikamalov, E., Couch, S. M., Haas, R., & Schnetter, E. (2016). NEUTRINO-DRIVEN CONVECTION IN CORE-COLLAPSE SUPERNOVAE: HIGH-RESOLUTION SIMULATIONS. The Astrophysical Journal, 820(1), 76. https://doi.org/10.3847/0004-637x/820/1/76 en_US
dc.identifier.issn 0004-637X
dc.identifier.uri https://iopscience.iop.org/article/10.3847/0004-637X/820/1/76
dc.identifier.uri https://doi.org/10.3847/0004-637X/820/1/76
dc.identifier.uri http://nur.nu.edu.kz/handle/123456789/4811
dc.description.abstract We present results from high-resolution semiglobal simulations of neutrino-driven convection in core-collapse supernovae. We employ an idealized setup with parameterized neutrino heating/cooling and nuclear dissociation at the shock front. We study the internal dynamics of neutrino-driven convection and its role in redistributing 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 downward 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 of 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 artifact. Kolmogorov scaling is progressively recovered as the resolution is increased. en_US
dc.language.iso en en_US
dc.publisher American Astronomical Society en_US
dc.relation.ispartofseries Astrophysical Journal;
dc.rights Attribution-NonCommercial-ShareAlike 3.0 United States *
dc.rights.uri http://creativecommons.org/licenses/by-nc-sa/3.0/us/ *
dc.subject proto-neutron star en_US
dc.subject PNS en_US
dc.subject core-collapse supernovae en_US
dc.subject CCSNe en_US
dc.subject Neutrino-driven Convection Model en_US
dc.subject Research Subject Categories::TECHNOLOGY en_US
dc.subject Research Subject Categories::NATURAL SCIENCES::Physics en_US
dc.title Neutrino-driven Convection in Core-collapse Supernovae: High-resolution Simulations en_US
dc.type Article en_US
workflow.import.source science

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