Abstract
We study several methods for timing the neutrino signal of a Galactic supernova (SN) for different detectors via Monte Carlo simulations. We find that, for the methods we studied, at a distance of $10\,$kpc both Hyper-Kamiokande and IceCube can reach precisions of $\sim1\,$ms for the neutrino burst, while a potential IceCube Gen2 upgrade will reach submillisecond precision. In the case of a failed SN, we find that detectors such as SK and JUNO can reach precisions of $\sim0.1\,$ms while HK could potentially reach a resolution of $\sim 0.01\,$ms so that the impact of the black hole formation process itself becomes relevant. Two possible applications for this are the triangulation of a (failed) SN as well as the possibility to constrain neutrino masses via a time-of-flight measurement using a potential gravitational wave signal as reference.
Highlights
Massive stars above ∼8 M⊙ most often end their lives in a great explosion outshining an entire galaxy for a short period of time
In the case of a failed SN, we find that detectors such as SK and JUNO can reach precisions of ∼0.1 ms while HK could potentially reach a resolution of ∼0.01 ms so that the impact of the black hole formation process itself becomes relevant
For such core-collapse supernovae (CCSNe), it is predicted that ∼99% of the released gravitational binding energy is emitted via neutrinos [1,2,3,4]
Summary
Massive stars above ∼8 M⊙ most often end their lives in a great explosion outshining an entire galaxy for a short period of time. In the case of a Galactic CCSN, the neutrino signal will reach us long before any optical signal can be detected This way it can serve as an early warning system (see SNEWS [12]). Besides other methods such as studying the statistics of neutrino-electron elastic scattering [13,14], the precise timing in multiple neutrino detectors can be used to locate the SN via triangulation [14,15,16,17,18].
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