SN 2024ggi的致密星周物质：另一颗具有爆炸前冒泡区和喷流驱动爆炸的超新星
The compact circumstellar material of SN 2024ggi: Another supernova with a pre-explosion effervescent zone and jet-driven explosion
AI总结：
本文研究了SN 2024ggi的致密星周物质，提出冒泡模型解释其CSM来源，并指出延迟中微子机制难以满足其高爆炸能量，从而支持抖动喷流爆炸机制（JJEM）。
摘要：
我研究了最近关于核坍缩超新星（CCSN）SN 2024ggi的最新理论和观测结果，发现其致密、紧凑的星周物质的可能解释是冒泡模型，在该模型中，气团或气流被恒星对流和脉动抬升后回落。该冒泡区与SN 2024ggi的红超巨星（RSG）前星体的常规星风并存。我发现，扩展的星风加速区在解释所需的CSM质量时存在一些困难。最近的建模发现SN 2024ggi的爆炸能量>1e51 erg，最高可达2e51 erg。我将此爆炸能量与最近关于延迟中微子爆炸机制的研究进行了对比，发现该机制在解释所需能量时可能存在一些困难。这可能表明爆炸是由抖动喷流爆炸机制（JJEM）引起的。这增加了支持JJEM的其他最新证据，特别是点对称的CCSN遗迹。
英文摘要：
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.
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