High-energy neutrino flux from SN2024ggi: constraints from semi-analytic modeling of its post-explosive emission

TL;DR

This paper models the high-energy neutrino emission from the nearby supernova SN2024ggi, linking electromagnetic and neutrino signals to constrain explosion parameters, and discusses implications for future multi-messenger observations.

Contribution

It introduces a semi-analytical model that connects electromagnetic and neutrino emissions in supernovae, enabling better interpretation of potential neutrino signals from such events.

Findings

Neutrino fluence peaks at TeV energies but is below current detector sensitivities.

The model constrains key explosion parameters like kinetic energy and ejecta mass.

Framework aids future detection strategies for nearby supernovae with next-generation observatories.

Abstract

Hydrogen-rich supernovae can efficiently accelerate particles when the expanding ejecta interact with the surrounding circumstellar medium (CSM), producing high-energy (TeV--PeV) neutrinos. In this work we investigate the nearby SN~2024ggi, whose proximity and clear signatures of ejecta--CSM interaction make it a promising candidate for studying high-energy ($\nu$) emission. We apply a new semi-analytical model that consistently links the electromagnetic and neutrino emission components, allowing us to constrain the main explosion parameters, including the kinetic energy, ejecta mass, progenitor radius, and nickel yield. The predicted high-energy ($\nu$) fluence at Earth peaks at TeV energies and remains below the sensitivity of current detectors. However, the modeling establishes a robust framework for interpreting future signals from nearby interacting supernovae and fine-tuning observational strategies for next-generation multi-messenger facilities such as IceCube-Gen2 and KM3NeT/ARCA.