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This study examines the feasibility of detecting neutrinos from binary neutron star mergers and using them to measure neutrino mass. The researchers find that current neutrino detectors are insufficient due to updated lower merger rates from LIGO/Virgo/KAGRA data and time-of-flight delays caused by neutrino mass, requiring future megaton-scale detectors like Deep-TITAND or MEMPHYS. By analyzing energy-dependent time windows following gravitational wave detection, they demonstrate that the timing difference between neutrino and gravitational wave arrivals could probe neutrino masses more sensitively than current terrestrial experiments like KATRIN or projected supernova-based measurements.
Why it matters
This research provides a novel astronomical method for measuring fundamental neutrino properties that could surpass laboratory-based techniques. The approach leverages the synergy between gravitational wave observatories and next-generation neutrino detectors, potentially resolving one of particle physics' key questions about the absolute neutrino mass scale.
arXiv:2511.16658v2 Announce Type: replace-cross
Abstract: Over the next decade, $mathcal{O}(100)$ diffuse supernova neutrino background (DSNB) events are expected in Hyper-Kamiokande. Another neutrino source that has received far less attention is binary neutron star mergers. Including the data from recent simulations, we find that detection in current and near-future neutrino experiments is not feasible, and a megaton-scale detector with $mathcal{O}(10)$ MeV threshold, such as the proposed Deep-TITAND, MEMPHYS, or MICA, will be required. This is due to the updated binary neutron star merger rate and the time-of-flight delay caused by the nonzero neutrino mass. Regarding the former, recent results from LIGO, Virgo, and KAGRA has significantly lowered the upper limit on the neutron star merger rate. As for the latter, neutrino events from neutron star mergers are expected to be recorded shortly after the gravitational wave signal. Limiting the analysis to such short time windows can significantly reduce background rates. While this approach has been qualitatively discussed in the literature, the effect of the time delay caused by neutrino mass, which can substantially extend the observation windows, has been disregarded. We present a refined analysis employing energy-dependent time windows and luminosity distance cuts for the mergers and provide realistic estimates of the detector runtime required to record neutrinos from binary neutron star mergers with small background contamination. The relative timing between the neutrino and gravitational wave signals can also be employed to probe the scale of neutrino mass. We find that the sensitivity to the lightest neutrino mass exceeds both the most stringent terrestrial bounds from KATRIN and the projections based on galactic supernovae. This level of sensitivity may become particularly relevant in the future if terrestrial and supernova constraints are not significantly improved.
Source: Prospects for Neutrino Observation and Mass Measurement from Binary Neutron Star Mergers