On the characteristics of fast neutrino flavor instabilities in three-dimensional core-collapse supernova models

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dc.contributor.authorAbbar, Sajaden
dc.contributor.authorCapozzi, Francescoen
dc.contributor.authorGlas, Roberten
dc.contributor.authorJanka, H-Thomasen
dc.contributor.authorTamborra, Ireneen
dc.contributor.departmentCenter for Neutrino Physicsen
dc.date.accessioned2021-07-30T17:13:24Zen
dc.date.available2021-07-30T17:13:24Zen
dc.date.issued2021-03-23en
dc.description.abstractWe assess the occurrence of fast neutrino flavor instabilities in two three-dimensional state-of-the-art core-collapse supernova simulations performed using a two-moment three-species neutrino transport scheme: one with an exploding 9M(circle dot) and one with a nonexploding 20M(circle dot) model. Apart from confirming the presence of fast instabilities occurring within the neutrino decoupling and the supernova pre-shock regions, we detect flavor instabilities in the post-shock region for the exploding model. These instabilities are likely to be scattering-induced. In addition, the failure in achieving a successful explosion in the heavier supernova model seems to seriously hinder the occurrence of fast instabilities in the post-shock region. This is a consequence of the large matter densities behind the stalled or retreating shock, which implies high neutrino scattering rates and thus more isotropic distributions of neutrinos and antineutrinos. Our findings suggest that the supernova model properties and the fate of the explosion can remarkably affect the occurrence of fast instabilities. Hence, a larger set of realistic hydrodynamical simulations of the stellar collapse is needed in order to make reliable predictions on the flavor conversion physics.en
dc.description.notesWe would like to thank Georg Raffelt for his comments on the manuscript and useful discussions. We acknowledge partial support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) through Grant Sonderforschungsbereich (Collaborative Research Center) SFB1258 "Neutrinos and Dark Matter in Astroand Particle Physics (NDM)". Additionally, F. C.'s work at Virginia Tech is supported by the U.S. Department of Energy under the Awards No. DE-SC0020250 and No. DE-SC0020262 and at Garching, funding by the European Research Council through Grant ERC-AdG No. 341157COCO2CASA and by DFG under Germany's Excellence Strategy through Cluster of Excellence ORIGINS (EXC2094)-390783311 is acknowledged. Computer resources for this project have been provided by the Leibniz Supercomputing Centre (LRZ) under LRZ project ID pr62za and by the Max Planck Computing and Data Facility (MPCDF) on the HPC system Hydra. I. T. acknowledges support fromthe Villum Foundation (Project No. 13164), the Danmarks Frie Forskningsfonds (Project No. 8049-00038B) and the Knud Ho jgaard Foundation.en
dc.description.sponsorshipDeutsche Forschungsgemeinschaft (DFG, German Research Foundation) through Grant Sonderforschungsbereich (Collaborative Research Center)German Research Foundation (DFG) [SFB1258]; U.S. Department of EnergyUnited States Department of Energy (DOE) [DE-SC0020250, DE-SC0020262]; European Research Council through Grant ERC-AdG [341157COCO2CASA]; DFG under Germany's Excellence Strategy through Cluster of Excellence ORIGINSGerman Research Foundation (DFG) [(EXC2094)-390783311]; Leibniz Supercomputing Centre (LRZ) under LRZ project [pr62za]; Max Planck Computing and Data Facility (MPCDF) on the HPC system Hydra; Villum Foundation [13164]; Danmarks Frie Forskningsfonds [8049-00038B]; Knud Ho jgaard Foundationen
dc.description.versionPublished versionen
dc.format.mimetypeapplication/pdfen
dc.identifier.doihttps://doi.org/10.1103/PhysRevD.103.063033en
dc.identifier.eissn2470-0029en
dc.identifier.issn2470-0010en
dc.identifier.issue6en
dc.identifier.other63033en
dc.identifier.urihttp://hdl.handle.net/10919/104460en
dc.identifier.volume103en
dc.language.isoenen
dc.rightsCreative Commons Attribution 4.0 Internationalen
dc.rights.urihttp://creativecommons.org/licenses/by/4.0/en
dc.titleOn the characteristics of fast neutrino flavor instabilities in three-dimensional core-collapse supernova modelsen
dc.title.serialPhysical Review Den
dc.typeArticle - Refereeden
dc.type.dcmitypeTexten
dc.type.dcmitypeStillImageen

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