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

Muhammad A. Latif, Dominik Schleicher

Research output: Contribution to journalArticlepeer-review

4 Citations (Scopus)

Abstract

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 at z = 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 × 105-7 107 M o˙. We find that a PISN evacuates the gas from halos ≤3 106 M o˙ and thereafter shuts off in situ star formation for at least 30 Myr. Pop II stellar clusters of 923 M o˙ and 6800 M o˙ form in halos of 3.8 × 107 M o˙ and 9 107 M o˙, 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 M o˙ yr-1, and the star formation efficiency is less than 1%.

Original languageEnglish
Article numberL31
JournalAstrophysical Journal Letters
Volume902
Issue number2
DOIs
Publication statusPublished - Oct 20 2020

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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