Abstract
Abstract Core-collapse supernovae are among the most magnificent events in the observable universe. They produce many of the chemical elements necessary for life to exist and their remnants—neutron stars and black holes—are interesting astrophysical objects in their own right. However, despite millennia of observations and almost a century of astrophysical study, the explosion mechanism of core-collapse supernovae is not yet well understood. Hyper-Kamiokande is a next-generation neutrino detector that will be able to observe the neutrino flux from the next galactic core-collapse supernova in unprecedented detail. We focus on the first 500 ms of the neutrino burst, corresponding to the accretion phase, and use a newly-developed, high-precision supernova event generator to simulate Hyper-Kamiokande's response to five different supernova models. We show that Hyper-Kamiokande will be able to distinguish between these models with high accuracy for a supernova at a distance of up to 100 kpc. Once the next galactic supernova happens, this ability will be a powerful tool for guiding simulations toward a precise reproduction of the explosion mechanism observed in nature.
Highlights
A star with a mass of at least 8 M typically dies in a corecollapse supernova
Number of events expected during the time interval of 20 ms to 520 ms for a supernova at the fiducial distance of 10 kpc (N10 kpc ) and the distances at which 100 or 300 events are expected in the inner detector of HyperKamiokande (d100 and d300, respectively) for the five supernova models considered in this work and for both normal and inverted mass ordering
We have generated data sets for the supernova models described in Section 3.1, for both normal and inverted mass ordering and for two different event counts per data set, as identified, this could in principle be used to further improve the model discrimination accuracy
Summary
A star with a mass of at least 8 M typically dies in a corecollapse supernova (ccSN). The electromagnetic emission from a ccSN begins minutes to hours after the initial explosion when the outgoing shock wave breaks through the surface of the star (Adams et al.2013) It is largely decoupled from the processes that occur during the explosion. Previous work has demonstrated that this would make it possible to identify whether the signal exhibits certain features like the standing accretion shock instability (SASI; Lund et al.2010; Tamborra et al 2013) or lepton-number emission selfsustained asymmetry (LESA; Tamborra et al 2014), or to characterize the stellar core, e.g., by determining its compactness (Horiuchi et al 2017) or the mass and radius of the resulting neutron star (Nakazato & Suzuki 2020). High-precision supernova event generator and a realistic detector simulation and event reconstruction, we
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