The Effect of Supernova Convection On Neutron Star and Black Hole Masses

被引：45

作者：

Fryer, Chris L. ^{[1
,2
,3
,4
,5
]}

Olejak, Aleksandra ^{[6
]}

Belczynski, Krzysztof ^{[6
]}

机构：

[1] Los Alamos Natl Lab, Ctr Theoret Astrophys, Los Alamos, NM 87545 USA

[2] Los Alamos Natl Lab, Comp Computat & Stat Sci Div, Los Alamos, NM 87545 USA

[3] Univ Arizona, Tucson, AZ 85721 USA

[4] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA

[5] George Washington Univ, Washington, DC 20052 USA

[6] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, 18 Bartycka St, PL-00716 Warsaw, Poland

来源：

ASTROPHYSICAL JOURNAL | 2022年 / 931卷 / 02期

关键词：

ROTATING MASSIVE STARS; GAMMA-RAY BURSTS; CORE-COLLAPSE; STELLAR EVOLUTION; ACCRETION; EXPLOSION; IMPACT; LIMITS; SOLAR; 1ST;

D O I：

10.3847/1538-4357/ac6ac9

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Our understanding of the convective-engine paradigm driving core-collapse supernovae has been used for two decades to predict the remnant mass distribution from stellar collapse. These predictions improve as our understanding of this engine increases. In this paper, we review our current understanding of convection (in particular, the growth rate of convection) in stellar collapse and study its effect on the remnant mass distribution. We show how the depth of the mass gap between neutron stars and black holes can help probe this convective growth. We include a study of the effects of stochasticity in both the stellar structure and the convective seeds caused by stellar burning. We study the role of rotation and its effect on the pair-instability mass gap. Under the paradigm limiting stellar rotation to those stars in tight binaries, we determine the effect of rotation on the remnant mass distribution.

引用

页数：13

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