Towards a universal analytical model for Population III star formation: interplay between feedback and fragmentation

被引：10

作者：

Liu, Boyuan ^{[1
,2
]}

Gurian, James ^{[3
]}

Inayoshi, Kohei ^{[4
]}

Hirano, Shingo ^{[5
]}

Hosokawa, Takashi ^{[6
]}

Bromm, Volker ^{[7
,8
]}

Yoshida, Naoki ^{[9
,10
,11
]}

机构：

[1] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[2] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, Albert Ueberle Str 2, D-69120 Heidelberg, Germany

[3] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada

[4] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China

[5] Univ Tokyo, Sch Sci, Dept Astron, Tokyo 1130033, Japan

[6] Kyoto Univ, Dept Phys, Sakyo, Kyoto 6068502, Japan

[7] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA

[8] Univ Texas Austin, Weinberg Inst Theoret Phys, Austin, TX 78712 USA

[9] Univ Tokyo, Sch Sci, Dept Phys, 7-3-1 Hongo, Bunkyo, Tokyo 1130033, Japan

[10] Univ Tokyo, Res Ctr Early Universe, Sch Sci, 7-3-1 Hongo, Bunkyo, Tokyo 1130033, Japan

[11] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2024年 / 534卷 / 01期

关键词：

stars: black holes; stars: Population III; dark ages; reionization; first stars; INITIAL MASS FUNCTION; BINARY BLACK-HOLES; M-CIRCLE-DOT; PULSATIONAL PAIR-INSTABILITY; SUPERMASSIVE PRIMORDIAL STARS; LYMAN-WERNER RADIATION; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT QUASARS; DARK-MATTER HALOES; HIGH-Z EXPLORATION;

D O I：

10.1093/mnras/stae2066

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

JWST has brought us new insights into Cosmic Dawn with tentative detection of the unique signatures of metal-free Population III (Pop III) stars, such as strong He II emission, extremely blue ultraviolet spectrum, and enhanced nitrogen abundance. Self-consistent theoretical predictions of the formation rates, sites, and masses of Pop III stars are crucial for interpreting the observations, but are challenging due to complex physical processes operating over the large range of length-scales involved. One solution is to combine analytical models for the small-scale star formation process with cosmological simulations that capture the large-scale physics such as structure formation, radiation backgrounds, and baryon-dark matter streaming motion that regulate the conditions of Pop III star formation. We build an analytical model to predict the final masses of Pop III stars/clusters from the properties of star-forming clouds, based on the key results of small-scale star formation simulations and stellar evolution models. Our model for the first time considers the interplay between feedback and fragmentation and covers different modes of Pop III star formation ranging from ordinary small (similar to 10-2000 M-circle dot) clusters in molecular-cooling clouds to massive (greater than or similar to 10(4) M-circle dot) clusters containing supermassive (similar to 10(4) - 3 x 10(5) M-circle dot) stars under violent collapse of atomic-cooling clouds with large gas accretion rates of greater than or similar to 0.1 M-circle dot yr(-1). As an example, the model is applied to the Pop III star-forming clouds in the progenitors of typical haloes hosting high-z luminous quasars (M-h similar to 10(12) M-circle dot at z similar to 6), which shows that formation of Pop III massive clusters is common (similar to 20-70 per cent) in such biased (similar to 4 sigma) regions, and the resulting heavy black hole seeds from supermassive stars can account for a significant fraction of observed luminous (greater than or similar to 10(46) erg s(-1)) quasars at z similar to 6.

引用

页码：290 / 312

页数：23

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