论文标题
原始黑洞合并速率在椭圆形 - 散发暗物质模型中
Primordial Black Hole Merger Rate in Ellipsoidal-Collapse Dark Matter Halo Models
论文作者
论文摘要
我们已经研究了光环的椭圆形散射模型中原始黑洞（PBH）的合并速率，以通过高级Ligo（Aligo）探测器从重力波检测中估算出的PBH合并的暗物质丰度。我们已经指出，对于椭圆形模型，每个光环中的PBH合并速率比球形模型更重要。我们已经指出，椭圆形折叠光环模型的每单位时间和每单位体积的PBH合并速率比相应的球形模型高约一个数量级。此外，我们已经计算了PBH总合并率随红移的函数的演变。结果表明，如模型所预期的那样，椭圆形光环模型的演变比球形光环模型更敏感。最后，在椭圆形和球形模型的背景下，我们对PBH丰度提出了限制。通过将结果与Aligo合并进行比较，在第三次观察过程中（O3），我们表明，椭圆形偏移晕模型中的合并速率落在Aligo窗口内，而相同的结果对于球形偏斜的结果无效。此外，我们已经比较了PBH的总合并率，这些PBH在椭圆形折叠halo模型中的分数中比较了几种PBHS。结果表明，PBHS的总合并率随质量成反比。我们还估计了PBH的分数与它们的质量在椭圆形折叠halo模型中的关系，并证明了PBHS的质量分布狭窄。结果表明，从PBH合并速率中推断出的椭圆形折叠halo模型的约束可能比球形浪潮曲面获得的相应结果可能更强大。
We have studied the merger rate of primordial black holes (PBHs) in the ellipsoidal-collapse model of halo to explain the dark matter abundance by the PBH merger estimated from the gravitational waves detections via the Advanced LIGO (aLIGO) detectors. We have indicated that the PBH merger rate within each halo for the ellipsoidal models is more significant than for the spherical models. We have specified that the PBH merger rate per unit time and per unit volume for the ellipsoidal-collapse halo models is about one order of magnitude higher than the corresponding spherical models. Moreover, we have calculated the evolution of the PBH total merger rate as a function of redshift. The results indicate that the evolution for the ellipsoidal halo models is more sensitive than spherical halo models, as expected from the models. Finally, we have presented a constraint on the PBH abundance within the context of ellipsoidal and spherical models. By comparing the results with the aLIGO mergers during the third observing run (O3), we have shown that the merger rate in the ellipsoidal-collapse halo models falls within the aLIGO window, while the same result is not valid for the spherical-collapse ones. Furthermore, we have compared the total merger rate of PBHs in terms of their fraction in the ellipsoidal-collapse halo models for several masses of PBHs. The results suggest that the total merger rate of PBHs changes inversely with their masses. We have also estimated the relation between the fraction of PBHs and their masses in the ellipsoidal-collapse halo model and have shown it for a narrow mass distribution of PBHs. The outcome shows that the constraint inferred from the PBH merger rate for the ellipsoidal-collapse halo models can be potentially stronger than the corresponding result obtained for the spherical-collapse ones.
