Where, when, and why: Occurrence of fast-pairwise collective neutrino oscillation in three-dimensional core-collapse supernova models

Nagakura, Hiroki; Burrows, Adam; Johns, Lucas; Fuller, George M.

doi:10.1103/physrevd.104.083025

Where, when, and why: Occurrence of fast-pairwise collective neutrino oscillation in three-dimensional core-collapse supernova models

Journal Article · Thu Oct 21 00:00:00 EDT 2021 · Physical Review. D.

DOI:https://doi.org/10.1103/physrevd.104.083025· OSTI ID:1979920

Nagakura, Hiroki ^[1]; ^[2]; ^[3]; Fuller, George M. ^[4]

Princeton University, NJ (United States); OSTI
Princeton University, NJ (United States)
University of California, Berkeley, CA (United States)
University of California, San Diego, La Jolla, CA (United States)

Fast-pairwise collective neutrino oscillation represents a key uncertainty in the theory of core-collapse supernova (CCSN). Despite the potentially significant impact on CCSN dynamics, it is usually neglected in numerical models of CCSN because of the formidable technical difficulties of self-consistently incorporating this physics. In this paper, we investigate the prospects for the occurrence of fast flavor conversion by diagnosing electron neutrino lepton number (ELN) crossing in more than a dozen state-of-the-art three-dimensional CCSN models. ELN crossings provide a necessary condition for triggering flavor conversion. Although only zeroth and first angular moments are available from the simulations, our new method enables us to look into the angular distributions of neutrinos in momentum space and provide accurate insight into ELN crossings. Our analysis suggests that fast flavor conversion generally occurs in the postshock region of CCSNe, and that explosive models provide more favorable conditions for the flavor conversion than failed CCSNe. Here we also find that there are both common and progenitor-dependent characteristics. Classifying ELN crossings into two types, we analyze the generation mechanism of each case by scrutinizing the neutrino radiation field and matter interactions. We find key ingredients of CCSN dynamics driving the ELN crossings: proto-neutron star convection, asymmetric neutrino emission, neutrino absorptions, and scatterings. This study suggests that we need to accommodate fast flavor conversions in realistic CCSN models.

View Accepted Manuscript (DOE)

Research Organization:: University of California, Oakland, CA (United States); Argonne National Laboratory (ANL), Argonne, IL (United States); University of California, San Diego, CA (United States)

Sponsoring Organization:: USDOE Office of Science (SC), Advanced Scientific Computing Research (ASCR); National Science Foundation (NSF); Princeton Institute for Computational Science and Engineering (PICSciE); National Aeronautics and Space Administration (NASA); Heising-Simons Foundation

Grant/Contract Number:: SC0018297; AC02-06CH11357; AC03-76SF00098

OSTI ID:: 1979920

Alternate ID(s):: OSTI ID: 1828814

Journal Information:: Physical Review. D., Journal Name: Physical Review. D. Journal Issue: 8 Vol. 104; ISSN 2470-0010

Publisher:: American Physical Society (APS)Copyright Statement

Country of Publication:: United States

Language:: English

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