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Neutrino flavour transformation in supernovae

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arxiv 0904.0974 v1 pith:KAYAOMA2 submitted 2009-04-06 astro-ph.HE hep-ph

Huaiyu Duan (INT , U of Washington) , James P Kneller (UMN , U of Paris-XI) This is my paper · ORCID
classification astro-ph.HEhep-ph
keywords flavourneutrinobeenmadeoscillationsprogresssupernovaeallow
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Rapid progress has been made during recent years in the understanding of the flavour oscillations that occur as neutrinos traverse through supernova. The previous paradigm has given way and it is now clear that the neutrino signals we shall receive from future Galactic supernovae will allow us both to peer inside these extraordinary cosmic events and to probe some of the fundamental properties of these elusive particles. In this review we aim to distill the progress that has been made focusing upon the effects of the dynamic density profile and the emergence of collective flavour oscillations due to neutrino self-interactions.

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Forward citations

Cited by 4 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 I. Homogeneous medium

    hep-ph 2024-12 accept novelty 8.0 of 10

    Slow neutrino flavor instabilities split into a new resonant small-scale branch with growth rate ~omega_E/epsilon and the familiar non-resonant branch with the traditional scale 1/sqrt(omega_E mu).

  2. Flavomons in Matter Gradients: Ray Tracing and Amplitude Evolution

    hep-ph 2026-04 unverdicted novelty 7.0 of 10

    Matter gradients slow but do not suppress neutrino-mass-induced flavor instabilities, so flavomon ray tracing is required instead of local stability analysis alone.

  3. Single-wave solutions of the neutrino fast flavor system. Part I. Mechanical properties

    hep-ph 2026-01 conditional novelty 6.0 of 10

    Single-wave neutrino flavor solutions form a non-integrable spin system without Gaudin invariants, so an exact flavor pendulum exists only for two beams and does not extend to continuous angle distributions.

  4. 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.

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