The compact circumstellar material of SN 2024ggi: Another supernova with a pre-explosion effervescent zone and jet-driven explosion

TL;DR

This paper investigates the dense circumstellar material of SN 2024ggi, proposing an effervescent model involving stellar convection and pulsation, and suggests a jet-driven explosion mechanism over neutrino-driven models.

Contribution

It introduces the effervescent model for CSM formation and discusses the potential jet-driven explosion mechanism for SN 2024ggi, challenging traditional neutrino-driven explanations.

Findings

Effervescent zone explains dense CSM better than wind models.

Explosion energy estimates support jet-driven mechanism.

Challenges for neutrino mechanism in explaining high explosion energy.

Abstract

I examine recent theoretical studies and observations of the recent core-collapse supernova (CCSN) SN 20224ggi and find that the likely explanation for its dense, compact circumstellar material is an effervescent model, where parcels or streams of gas are uplifted by stellar convection and pulsation and fall back. The effervescent zone exists alongside the regular wind from the red supergiant (RSG) progenitor of SN 2024ggi. I find that an extended wind-acceleration zone encounters some difficulties in accounting for the required CSM mass. Recent modelling finds the explosion energy of SN 2024ggi to be >1e51 erg, and up to 2e51 erg. I examine this explosion energy against a recent study of the delayed neutrino explosion mechanism and find that this mechanism might have some difficulties in accounting for the required energy. This might suggest that the explosion was caused by the jittering jets explosion mechanism (JJEM). This adds to other recent pieces of evidence supporting the JJEM, particularly point-symmetric CCSN remnants.