期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 852, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/2041-8213/aaa28c
关键词
methods: numerical; stars: black holes; stars: massive; supernovae: general
资金
- Australian Government
- Government of Western Australia
- ARC grants [FT120100363]
- STFC grant [ST/P000312/1]
- JINA-CEE through US NSF grant [PHY-1430152]
- European Research Council through ERC-StG grant [EXAGAL-308037]
- Direct For Mathematical & Physical Scien [1430152] Funding Source: National Science Foundation
Fallback in core-collapse supernovae is considered a major ingredient for explaining abundance anomalies in metal-poor stars and the natal kicks and spins of black holes (BHs). We present a first 3D simulation of BH formation and fallback in an aborted neutrino-driven explosion of a 40 solar mass zero-metallicity progenitor from collapse to shock breakout. We follow the phase up to BH formation using the relativistic COCONUT-FMT code. For the subsequent evolution to shock breakout we apply the moving-mesh code AREPO to core-collapse supernovae for the first time. Our simulation shows that despite early BH formation, neutrino-heated bubbles can survive for tens of seconds before being accreted, leaving them sufficient time to transfer part of their energy to sustain the shock wave as is propagates through the envelope. Although the initial net energy (similar to 2 Bethe) of the neutrino-heated ejecta barely equals the binding energy of the envelope, 11 M circle dot of hydrogen are still expelled with an energy of 0.23 Bethe. We find no significant mixing and only a modest BH kick and spin, but speculate that stronger effects could occur for slightly more energetic explosions or progenitors with less tightly bound envelopes.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据