High-energy gamma-ray and neutrino emissions from interacting supernovae based on radiation hydrodynamic simulations: a case of SN 2023ixf

TL;DR

This study models gamma-ray and neutrino emissions from supernova SN 2023ixf, revealing that cosmic-ray acceleration occurs days after explosion and is constrained by observations, highlighting the importance of multi-messenger astronomy.

Contribution

The paper presents radiation-hydrodynamic simulations of supernova ejecta interacting with dense CSM, predicting high-energy emissions and constraining cosmic-ray production efficiency.

Findings

CR acceleration begins around 4 days post-explosion

Gamma-ray and neutrino emissions peak approximately 9 days after explosion

Cosmic-ray production efficiency is constrained to be less than 10%

Abstract

Recent observations of core-collapse supernovae revealed that the existence of dense circumstellar matter (CSM) around their progenitors is ubiquitous. Interaction of supernova ejecta with such a dense CSM is a potential production sight of high-energy cosmic rays (CRs), gamma-rays, and neutrinos. We estimate the gamma-ray and neutrino signals from SN 2023ixf, a core-collapse supernova occurred in a nearby galaxy M101, which exhibits signatures of the interaction with the confined dense CSM. Using radiation-hydrodynamic simulation model calibrated by the optical and ultraviolet observations of SN 2023ixf, we find that the CRs cannot be accelerated in the early phase because the sharp velocity jump at the shock disappears due to strong radiation pressure. Roughly 4 days after the explosion, the collisionless sub-shock is formed in the CSM, which enables the CR production and leads to gamma-ray and neutrino emissions. The shock sweeps up the entire dense CSM roughly 9 days after the explosion, which ceases the high-energy radiation. Based on this scenario, we calculate the gamma-ray and neutrino signals, which have a peak around 9 days after the explosion. We can constrain the cosmic-ray production efficiency to be less than 10% by comparing our prediction to the Fermi-LAT upper limits. Future multi-messenger observations with an enlarged sample of nearby supernovae will provide a better constraint on the cosmic-ray production efficiency in the early phases of supernovae.