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Neutrino flavor instabilities: onset and development

Goimil García, Manuel

Publisher
Zenodo
DOI
10.5281/zenodo.17696052
Repository
zenodo.org
Language
en

Abstract

Parallel talk presented at the XXI International Workshop on Neutrino Telescopes - Padova 29 September - 3 October 2025 (https://agenda.infn.it/event/44606/) Abstract: At high enough neutrino densities, the phenomenology of flavor conversion may be governed by neutrino-neutrino coherent forward scattering. In contrast to neutral current scattering on charged leptons, this process can be flavor-changing. The coherent nature of the interaction then implies that a large amount of neutrinos can undergo flavor conversion simultaneously. This collective effect is prone to runaway modes, which can change the flavor content of a neutrino ensemble on very short time scales. Capturing these instabilities is crucial in order to accurately model the large-scale dynamics of compact astrophysical objects. In this talk, I will describe the appearance and evolution of collective flavor instabilities in simple models of neutrino-dense media and provide simple recipes to predict the final flavor configuration. Funded by the European Research Council - European Union.

Full text

Neutrino flavor instabilities: onset and development Manuel Goimil García XXI International Workshop on Neutrino Telescopes 01/10/25 Outline ➢Neutrino flavor conversion in core-collapse supernovae ➢Model of neutrino self-interactions ➢Results: ○How do self-interactions behave? ○How do we predict their outcome? ➢Conclusions Based on M. Goimil-García and I. Tamborra, Phys. Rev. D 112, 10 2 Introduction (1): neutrino flavor conversion Vacuum oscillations Refraction in matter 3 Introduction (2): self-induced flavor conversion Neutrino-neutrino refraction Collective flavor instability 4 Introduction (3): core-collapse supernovae From I. Tamborra, Nature Rev. Phys. 7 (2025) nν~1034–35 cm-3 nbaryon~1036 cm-3 νν refraction can help or hinder supernova explosions Ehring et al., Phys. Rev. Lett. 131 (2023) MPA Supernova Archive, Bollig (2016) 5 Model of self-interactions (1) ➢(Anti)neutrino equations of motion: Hamiltonian (function of D) Lepton number (LN) polarization vector: [ELN–XLN] Flavor coherence Can we predict the neutrino survival probabilities? Advection 6 Model of self-interactions (2) Suite of homogeneous backgrounds Inhomogeneous perturbation 7 Results (1): Impact of advection on flavor instabilities Neutrino densities Advection spreads the perturbation and destroys quasi-periodic behavior Initial perturbation at r=450μ-1 8 Results (1): Impact of advection on flavor instabilities 9