  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 has difficulties in accounting for the required energy. This suggests
that the explosion was caused by the jittering jets explosion mechanism (JJEM),
adding to other recent pieces of evidence supporting the JJEM, particularly
point-symmetric CCSN remnants.
