论文标题
$ n $ body模拟中原始黑孔的聚类动力学
The clustering dynamics of primordial black boles in $N$-body simulations
论文作者
论文摘要
我们探讨了暗物质（DM）可以通过大约原始黑洞（PBH）的恒星质量群集的不均匀背景来解释的可能性，该背景使用牛顿$ n $ n $ code模拟了从重组到现在的5000多个实现的进化。我们计算蒸发的簇率，并提取二进制和合并的子人群以及其父母和合并树历史，寿命和地层率；动力学和轨道参数曲线，质量分离和动力学摩擦的程度以及近距离相遇的功率谱。总体而言，我们发现PBHS可以构成一个可行的DM候选人，并且它们的聚类在整个宇宙历史上呈现出丰富的现象学。我们表明，二进制系统目前约占所有PBH的9.5％，质量比为$ \ bar {q} _ {\ rm b} = 0.154 $，总质量为$ \ bar {m} _ {\ rm t，\ rm t，\ b} = 303 = 303 = 303 \ \，m _ \ osot $。合并的PBH是罕见的，目前所有PBH的约0.0023 \％，质量比为$ \ bar {q} _ {\ rm b} = 0.965 $，总质量为$ \ bar {m} _ {m} _ {\ rm t { \ bar {m} _ {c，{\ rm m}}} = 642 \，m_ \ odot $。我们发现，聚集膨胀和蒸发会导致这些pBH的气泡1 kpc，目前包含约36 \％的物体和质量，有数百个PC大小的核。我们还发现，这些PBH子途径分布在数百个KPC的较宽的PBH光环中，其中包含约63％的物体和质量，与银河系光环的大小相吻合。我们最终发现，大量黑洞的紧密相遇（$ m \ sim 1000 \，m_ \ odot $），带有$γ^{\ mathrm {s}} =（1.2^{+5.9} _ { - 0.9} _ { - 0.9}）与$γ^{\ mathrm {m}} = 1337 \ pm 41 \ mathrm {yr^{ - 1} gpc^{ - 3}} $合并。
We explore the possibility that Dark Matter (DM) may be explained by a non-uniform background of approximately stellar-mass clusters of Primordial Black Holes (PBHs), by simulating the evolution them from recombination to the present with over 5000 realisations using a Newtonian $ N $-body code. We compute the cluster rate of evaporation, and extract the binary and merged sub-populations along with their parent and merger tree histories, lifetimes and formation rates; the dynamical and orbital parameter profiles, the degree of mass segregation and dynamical friction, and power spectrum of close encounters. Overall, we find that PBHs can constitute a viable DM candidate, and that their clustering presents a rich phenomenology throughout the history of the Universe. We show that binary systems constitute about 9.5\% of all PBHs at present, with mass ratios of $ \bar{q}_{\rm B} = 0.154 $, and total masses of $ \bar{m}_{\rm T,\,B} = 303\,M_\odot$. Merged PBHs are rare, about 0.0023\% of all PBHs at present, with mass ratios of $ \bar{q}_{\rm B}= 0.965 $ with total and chirp masses of $ \bar{m}_{\rm T,\,B}= 1670\,M_\odot$ and $ \bar{m}_{c,{\rm M}} = 642\,M_\odot $ respectively. We find that cluster puffing up and evaporation leads to bubbles of these PBHs of order 1 kpc containing at present times about 36\% of objects and mass, with hundred pc sized cores. We also find that these PBH sub-haloes are distributed in wider PBH haloes of order hundreds of kpc, containing about 63\% of objects and mass, coinciding with the sizes of galactic halos. We find at last high rates of close encounters of massive Black Holes ($ M \sim 1000\,M_\odot$), with $ Γ^{\mathrm{S}} = (1.2^{+5.9}_{-0.9}) \times 10^{7} \mathrm{yr^{-1} Gpc^{-3}}$ and mergers with $Γ^{\mathrm{M}} = 1337 \pm 41 \mathrm{yr^{-1} Gpc^{-3}} $.
