Neutrino Flavor Conversion Shapes the Rate of Failed Core-collapse Supernovae
Abstract
The relative rate of neutron stars and black holes produced by the collapse of massive stars is highly uncertain. We simulate the stellar collapse of $195$ progenitors with masses between 9 M⊙ and 120 M⊙, incorporating a schematic treatment of neutrino flavor conversion. We find that flavor transformation reshapes the explodability of massive stars-especially in the $16−30\, M_\odot$ mass range-and modifies the compact remnant mass distribution. Our findings identify neutrino flavor conversion as a fundamental ingredient in predicting neutron star and black hole populations, while naturally easing the red-supergiant and the supernova-rate problems, as well as reconciling theoretical expectations with the low-mass tail of the observed neutron star mass distribution.
Versions
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BibTeX
@misc{gogilashvili2026neutrino,
title = {{Neutrino Flavor Conversion Shapes the Rate of Failed Core-collapse Supernovae}},
author = {Mariam Gogilashvili and Irene Tamborra},
howpublished = {arXiv},
year = {2026},
month = aug,
doi = {10.48550/arxiv.2605.16504},
eprint = {2605.16504},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2605.16504},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Neutrino Flavor Conversion Shapes the Rate of Failed Core-collapse Supernovae
AU - Mariam Gogilashvili
AU - Irene Tamborra
PY - 2026
DA - 2026/08/18
PB - arXiv
DO - 10.48550/arxiv.2605.16504
UR - https://arxiv.org/abs/2605.16504
AB - The relative rate of neutron stars and black holes produced by the collapse of massive stars is highly uncertain. We simulate the stellar collapse of $195$ progenitors with masses between 9 M_⊙ and 120 M_⊙, incorporating a schematic treatment of neutrino flavor conversion. We find that flavor transformation reshapes the explodability of massive stars-especially in the $16−30\, M_\odot$ mass range-and modifies the compact remnant mass distribution. Our findings identify neutrino flavor conversion as a fundamental ingredient in predicting neutron star and black hole populations, while naturally easing the red-supergiant and the supernova-rate problems, as well as reconciling theoretical expectations with the low-mass tail of the observed neutron star mass distribution.
ER -