Neutrino-Mass-Driven Instabilities as the Earliest Flavor Conversion in Supernovae
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| Format: | Preprint |
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2025
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| _version_ | 1866908666269007872 |
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| author | Fiorillo, Damiano F. G. Janka, Hans-Thomas Raffelt, Georg G. |
| author_facet | Fiorillo, Damiano F. G. Janka, Hans-Thomas Raffelt, Georg G. |
| contents | Collective neutrino flavor conversions in core-collapse supernovae (SNe) begin with instabilities, initially triggered when the dominant $ν_e$ outflow concurs with a small antineutrino flux of opposite lepton number, with $\overlineν_e$ dominating over $\overlineν_μ$. When these "flipped" neutrinos emerge in the energy-integrated angular distribution (angular crossing), they initiate a fast instability. However, before such conditions arise, spectral crossings typically appear within $20~\mathrm{ms}$ of collapse, i.e., local spectral excesses of $\overlineν_e$ over $\overlineν_μ$ along some direction. Therefore, post-processing SN simulations cannot consistently capture later fast instabilities because the early slow ones have already altered the conditions. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2507_22985 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Neutrino-Mass-Driven Instabilities as the Earliest Flavor Conversion in Supernovae Fiorillo, Damiano F. G. Janka, Hans-Thomas Raffelt, Georg G. High Energy Physics - Phenomenology Cosmology and Nongalactic Astrophysics High Energy Astrophysical Phenomena Collective neutrino flavor conversions in core-collapse supernovae (SNe) begin with instabilities, initially triggered when the dominant $ν_e$ outflow concurs with a small antineutrino flux of opposite lepton number, with $\overlineν_e$ dominating over $\overlineν_μ$. When these "flipped" neutrinos emerge in the energy-integrated angular distribution (angular crossing), they initiate a fast instability. However, before such conditions arise, spectral crossings typically appear within $20~\mathrm{ms}$ of collapse, i.e., local spectral excesses of $\overlineν_e$ over $\overlineν_μ$ along some direction. Therefore, post-processing SN simulations cannot consistently capture later fast instabilities because the early slow ones have already altered the conditions. |
| title | Neutrino-Mass-Driven Instabilities as the Earliest Flavor Conversion in Supernovae |
| topic | High Energy Physics - Phenomenology Cosmology and Nongalactic Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2507.22985 |