论文标题
在一对不稳定性超新星之后，流行II星簇的形成
Formation of Pop II star clusters in the aftermath of a pair instability supernova
论文作者
论文摘要
在大爆炸之后，流行II明星是宇宙电力的关键动力和高红移星系的组成部分。这些恒星形成如何以及何时是正在进行的研究的主题。我们进行宇宙辐射流体动力学模拟，以研究在$ z = 10-25 $的暗物质晕在$ z = 10-25 $的情况下的形成。我们的模拟以自洽的方式对流行III和POP II恒星的形成以及它们的辐射，化学和SN反馈在$ \ rm 5 \ times 10^5- 7 \ times 10^7〜m _ {\ odot} $中的散发性，化学和SN反馈。我们发现，PISN从Halos $ \ rm \ rm \ leq 3 \ times 10^{6} 〜M _ {\ odot} $中撤离气体，此后关闭了原位星形成，以30 Myr的位置。 $ \ rm 923〜m _ {\ odot} $和$ \ rm 6800〜m _ {\ odot} $形式为$ \ rm 3.5 \ rm 3.5 \ times 10^7〜m _ {\ odot} $ _ {\ odot} $ _ 2^7〜M _ 7〜RM 7.2 \ rm 7.2，恒星形成的模式高度发作性，主要由POP II SN反馈调节。平均恒星形成率为$ \ rm 10^{ - 5} -10^{ - 4} 〜m _ {\ odot}/yr $，而星形的效率小于1 \％。
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 Pop III and Pop II stars in a self-consistent manner along with their radiative, chemical and SN feedback in halos of $\rm 5 \times 10^5- 7 \times 10^7~M_{\odot}$. We find that a PISN evacuates the gas from halos $\rm \leq 3 \times 10^{6}~M_{\odot}$ and thereafter shuts off in situ star formation for at-least 30 Myr. Pop II stellar clusters of $\rm 923~M_{\odot}$ and $\rm 6800~M_{\odot}$ form in halos of $\rm 3.5 \times 10^7~M_{\odot}$ and $\rm 7.2 \times 10^7~M_{\odot}$, respectively. The mode of star formation is highly episodic and mainly regulated by Pop II SN feedback. The average star formation rates are $\rm 10^{-5}-10^{-4}~M_{\odot}/yr$ and the star formation efficiency is less than 1\%.
