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

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dc.contributor.authorRadice, David
dc.contributor.authorOtt, Christian D.
dc.contributor.authorAbdikamalov, Ernazar
dc.contributor.authorCouch, Sean M.
dc.contributor.authorHaas, Roland
dc.contributor.authorSchnetter, Erik
dc.date.accessioned2020-06-26T11:03:40Z
dc.date.available2020-06-26T11:03:40Z
dc.date.issued2016-03
dc.description.abstractWe 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.identifier.citationRadice, 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/820/1/76en_US
dc.identifier.issn0004-637X
dc.identifier.urihttps://iopscience.iop.org/article/10.3847/0004-637X/820/1/76
dc.identifier.urihttps://doi.org/10.3847/0004-637X/820/1/76
dc.identifier.urihttp://nur.nu.edu.kz/handle/123456789/4811
dc.language.isoenen_US
dc.publisherAmerican Astronomical Societyen_US
dc.relation.ispartofseriesAstrophysical Journal;
dc.rightsAttribution-NonCommercial-ShareAlike 3.0 United States*
dc.rights.urihttp://creativecommons.org/licenses/by-nc-sa/3.0/us/*
dc.subjectproto-neutron staren_US
dc.subjectPNSen_US
dc.subjectcore-collapse supernovaeen_US
dc.subjectCCSNeen_US
dc.subjectNeutrino-driven Convection Modelen_US
dc.subjectResearch Subject Categories::TECHNOLOGYen_US
dc.subjectResearch Subject Categories::NATURAL SCIENCES::Physicsen_US
dc.titleNeutrino-driven Convection in Core-collapse Supernovae: High-resolution Simulationsen_US
dc.typeArticleen_US
workflow.import.sourcescience

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