Formation of Population II Star Clusters in the Aftermath of a Pair Instability Supernova
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%.
|Título según WOS:||Formation of Population II Star Clusters in the Aftermath of a Pair Instability Supernova|
|Título de la Revista:||ASTROPHYSICAL JOURNAL LETTERS|
|Editorial:||IOP PUBLISHING LTD|
|Fecha de publicación:||2020|