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Simulations of Fast Neutrino Flavor Conversions with Interactions in Inhomogeneous Media

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arxiv 2109.00091 v2 pith:IAUKTAS7 submitted 2021-08-31 hep-ph astro-ph.HE

Guenter Sigl This is my paper · ORCID
classification hep-phastro-ph.HE
keywords neutrinocurrentfastflavormediumscatteringtermsbackground
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We investigate toy models for spatial and temporal instabilities in collective neutrino oscillations induced by neutrino self-interactions, with special emphasis on inhomogeneous systems with densities following a profile. Simulations are based on a mathematica program that solves the Liouville equation with or without vacuum terms, refractive terms from a background medium, and neutrino-neutrino forward scattering, in one space dimension and in time. A discrete number of momentum modes are characterized by the neutrino velocity projection on the spatial direction. We also consider the effects of charged current interaction source terms and neutral current scattering contributions. We find that refractive effects from the medium, in particular for density distributions with a profile, and neutral current non-forward scattering off the background medium can strongly influence fast collective flavor transformations. Specifically we find that if both are present, fast flavor conversions can be strongly suppressed or at least delayed.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Theory of neutrino slow flavor evolution. Part II. Space-time evolution of linear instabilities

    hep-ph 2025-01 conditional novelty 6.0 of 10

    All weak fast and slow neutrino flavor instabilities are convective, so they grow spatially along neutrino directions rather than locally in time.

  2. Estimating amplitude of matter density fluctuations in solar and supernova models using neutrino flavor evolution

    astro-ph.HE 2026-07 conditional novelty 5.0 of 10

    SDA recovers density-fluctuation amplitudes from boundary neutrino flavor data in simplified solar and CCSN models, more reliably for the Sun and at high noise in CCSN.

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