Neutrinos have been a topic of significant interest due to their small mass, oscillatory behavior, and weak interaction with ordinary matter, making their detection a substantial challenge. This requires the use of large water tanks and photosensitive detectors to capture Cherenkov radiation. Supernovae, which are energetic events occurring at the end of stellar evolution from the core collapse of stars exceeding 10 solar masses, release a vast majority of their energy in the form of neutrinos. Detecting these neutrinos is crucial to understanding the mechanisms behind stellar death. Experiments like Hyper-Kamiokande (HK), a next-generation detector, are designed to study both supernova formation and neutrino properties.

This work aims to simulate the response of HK to different supernova models using event generation software (sntools) and detector simulation (WCSim). We will employ five supernova models to analyze the neutrino flux and differentiate between the models. The focus is on the first 520 milliseconds of the event, corresponding to the accretion phase, with distances greater than 77 kpc, to demonstrate the detector's sensitivity and efficiency in capturing data.