Neutrinos, fundamental particles with extremely small masses, exhibit unique properties such as flavor oscillation and weak interaction with ordinary matter, which makes their detection challenging. This has led to the development of large-volume detectors, such as ultrapure water tanks equipped with photosensitive sensors capable of registering Cherenkov radiation. On the other hand, supernovae—highly energetic events associated with the core collapse of stars with more than 10 solar masses (Type II) or the explosion of white dwarfs (Type Ia)—emit part of their energy in the form of neutrinos, making them privileged natural sources for the study of these particles. In this context, next-generation detectors such as Hyper-Kamiokande represent key tools for investigating both the formation mechanisms of supernovae and the fundamental properties of neutrinos.

The objective of this work is to simulate the response of the Hyper-Kamiokande detector to different neutrino emission models from supernovae. Four Type II supernova models will be analyzed, focusing the study on the first 520 milliseconds of the event, corresponding to the accretion phase, as well as two Type Ia supernova models. Through numerical analysis of the simulated data, the experiment's ability to discriminate between the different models will be evaluated, thus providing relevant information on the feasibility of using neutrino observations to characterize extreme astrophysical events.

sergio.galarza@ms.uas.edu.mx

Sergio de Jesus Galarza Ballesteros