Fast-pairwise Collective Neutrino Oscillations Associated with Asymmetric Neutrino Emissions in Core-collapse Supernovae

Nagakura, Hiroki; Morinaga, Taiki; Kato, Chinami; Yamada, Shoichi

doi:10.3847/1538-4357/ab4cf2

Title: Fast-pairwise Collective Neutrino Oscillations Associated with Asymmetric Neutrino Emissions in Core-collapse Supernovae

Journal Article · Fri Nov 29 00:00:00 EST 2019 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/ab4cf2· OSTI ID:1803349

^[1]; Morinaga, Taiki ^[2];

^[3];

^[2]

Princeton Univ, Princeton, NJ (United States). Dept. of Astrophysical Sciences
Waseda Univ., Tokyo (Japan). Dept. of Science and Engineering
Tohoku Univ. (Japan). Dept. of Aerospace Engineering

We present a linear stability analysis of the fast-pairwise neutrino flavor conversion based on a result of our latest axisymmetric core-collapse supernova (CCSN) simulation with full Boltzmann neutrino transport. In the CCSN simulation, coherent asymmetric neutrino emissions of electron-type neutrinos (νe) and their antiparticles ($$\bar{v}$$e), in which the asymmetries of νe and $$\bar{v}$$e are anticorrelated with each other, occur at almost the same time as the onset of aspherical shock expansion. We find that the asymmetric neutrino emissions play a crucial role on occurrences of fast flavor conversions. The linear analysis shows that unstable modes appear in both pre- and post-shock flows; for the latter, they appear only in the hemisphere of higher $$\bar{v}$$e emissions (the same hemisphere with stronger shock expansion). We analyze the characteristics of electron–lepton number (ELN) crossing in depth by closely inspecting the angular distributions of neutrinos in momentum space. The ELN crossing happens in various ways, and the property depends on the radius: in the vicinity of neutron star, $$\bar{v}$$e (νe) dominates over ve ($$\bar{n}$$e) in the forward (backward) direction; at the larger radius, the ELN crossing occurs in the opposite way. We also find that the non-radial ELN crossing occurs at the boundary between no ELN crossing and the radial one, which is an effect of genuine multi-dimensional transport. Our findings indicate that the collective neutrino oscillation may occur more commonly in CCSNe and suggest that the CCSN community needs to accommodate these oscillations self-consistently in the modeling of CCSNe

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Research Organization:: Univ. of California, Oakland, CA (United States)

Sponsoring Organization:: USDOE Office of Science (SC)

Grant/Contract Number:: SC0018297

OSTI ID:: 1803349

Journal Information:: The Astrophysical Journal (Online), Vol. 886, Issue 2; ISSN 1538-4357

Publisher:: IOP PublishingCopyright Statement

Country of Publication:: United States

Language:: English

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79 ASTRONOMY AND ASTROPHYSICS
Astronomy & Astrophysics
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Neutrino oscillations
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