Formation of Population II Star Clusters in the Aftermath of a Pair Instability Supernova

被引：8

作者：

Latif, Muhammad A. ^{[1
]}

Schleicher, Dominik ^{[2
]}

机构：

[1] United Arab Emirates Univ, Coll Sci, Phys Dept, POB 15551, Al Ain, U Arab Emirates

[2] Barrio Univ, Univ Concepcion, Astron Dept, Concepcion, Chile

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2020年 / 902卷 / 02期

关键词：

Population III stars; Population II stars; Supernovae; Cosmology; Star formation; Star-forming regions; High-redshift galaxies; LOW-METALLICITY; FRAGMENTATION; EVOLUTION; GALAXIES; FEEDBACK;

D O I：

10.3847/2041-8213/abbdad

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Population II (Pop II) stars formed a few hundred million years after the Big Bang were key drivers of cosmic reionization and building blocks of high-redshift galaxies. How and when these stars formed is a subject of ongoing research. We conduct cosmological radiation hydrodynamical simulations to investigate the formation of Pop II star clusters in dark matter halos forming atz = 10-25 in the aftermath of a pair instability supernova (PISN). Our simulations model the formation of Population III and Pop II stars in a self-consistent manner along with their radiative, chemical, and SN feedback in halos of 5 x 10(5)-7 x 10(7)M. We find that a PISN evacuates the gas from halos <= 3 x 10(6)Mand thereafter shuts off in situ star formation for at least 30 Myr. Pop II stellar clusters of 923Mand 6800Mform in halos of 3.8 x 10(7)Mand 9 x 10(7)M, respectively. The mode of star formation is highly episodic and mainly regulated by Pop II SN feedback. The average star formation rates are 10(-5)-10(-4)Myr(-1), and the star formation efficiency is less than 1%.

引用

页数：7

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