标题： 模拟中间质量黑洞的增长 显示英文标题

标题： Simulating the growth of Intermediate Mass Black Holes

摘要： Theoretical models predict that a population of Intermediate Mass Black Holes (IMBHs) of mass $M_\bullet \approx 10^{4-5} \, \mathrm{M_{\odot}}$ might form at high ($z > 10$) redshift by different processes. Such objects would represent the seeds out of which $z > 6$ Super-Massive Black Holes (SMBHs) grow. We numerically investigate the radiation-hydrodynamic evolution governing the growth of such seeds via accretion of primordial gas within their parent dark matter halo of virial temperature $T_{vir} \sim 10^4 \, \mathrm{K}$. 我们发现，质量初始为$M_0=10^5 \, \mathrm{M_{\odot}}$的直接坍缩黑洞 (DCBH) 的吸积过程以平均速率$\dot{M}_{\bullet} \simeq 1.35 \, \dot{M}_{Edd} \simeq 0.1 \, \mathrm{M_{\odot} \, yr^{-1}}$发生，且是间歇性的（ duty-cycle 为$ < 50\%$），持续时间为$\approx 142 \, \mathrm{Myr}$；该系统平均以超爱丁顿亮度辐射，随着向中心天体直接供能的内层质量壳密度增加，其亮度逐渐增强。 最终，当气体总质量的$\approx 90\%$被吸积到黑洞上后（尽管平均辐射超过爱丁顿极限），黑洞最终质量达到$\sim 7 \times 10^6 \, \mathrm{M_{\odot}}$，剩余的气体由于强烈的辐射爆发被从星系晕中吹走，峰值亮度达到$L_{peak}\sim 3\times 10^{45} \, \mathrm{erg \, s^{-1}}$。 在大部分演化过程中，IMBH 是康普顿厚的，在模拟的后期阶段达到柱密度$N_H \sim 10^{25} \, \mathrm{cm^{-2}}$。 我们简要讨论了该模型的观测影响。 显示英文摘要

摘要： Theoretical models predict that a population of Intermediate Mass Black Holes (IMBHs) of mass $M_\bullet \approx 10^{4-5} \, \mathrm{M_{\odot}}$ might form at high ($z > 10$) redshift by different processes. Such objects would represent the seeds out of which $z > 6$ Super-Massive Black Holes (SMBHs) grow. We numerically investigate the radiation-hydrodynamic evolution governing the growth of such seeds via accretion of primordial gas within their parent dark matter halo of virial temperature $T_{vir} \sim 10^4 \, \mathrm{K}$. We find that the accretion onto a Direct Collapse Black Hole (DCBH) of initial mass $M_0=10^5 \, \mathrm{M_{\odot}}$ occurs at an average rate $\dot{M}_{\bullet} \simeq 1.35 \, \dot{M}_{Edd} \simeq 0.1 \, \mathrm{M_{\odot} \, yr^{-1}}$, is intermittent (duty-cycle $ < 50\%$) and lasts $\approx 142 \, \mathrm{Myr}$; the system emits on average at super-Eddington luminosities, progressively becoming more luminous as the density of the inner mass shells, directly feeding the central object, increases. Finally, when $\approx 90\%$ of the gas mass has been accreted (in spite of an average super-Eddington emission) onto the black hole, whose final mass is $\sim 7 \times 10^6 \, \mathrm{M_{\odot}}$, the remaining gas is ejected from the halo due to a powerful radiation burst releasing a peak luminosity $L_{peak}\sim 3\times 10^{45} \, \mathrm{erg \, s^{-1}}$. The IMBH is Compton-thick during most of the evolution, reaching a column density $N_H \sim 10^{25} \, \mathrm{cm^{-2}}$ in the late stages of the simulation. We briefly discuss the observational implications of the model.