AI 中文总结
研究恒星质量范围内原初黑洞双星轨道偏心率，通过模拟大量样本追踪其轨道演化，计算相关参数。发现孤立演化双星在多数频段会完全圆化，暗物质晕中的双星偏心率可能更高。预测LISA和DECIGO可探测一定数量偏心双星，排除它们能提高PBH丰度限制。
AI 中文摘要
恒星质量范围内的原初黑洞（PBH）双星仍可能是LIGO和未来引力波（GW）天文台可探测的致密天体双星的一部分。形成时的PBH双星通常具有很高的偏心率。本文研究了所有形成渠道的恒星质量范围内PBH双星的偏心率，并考虑了所有演化路径。我们模拟了大量PBH双星样本，追踪它们直至合并或至今的完整轨道演化。对于合并的双星，我们计算了它们的GW应变、可探测性以及LISA、DECIGO、ET、CE和aLIGO的偏心率分布。我们发现，孤立演化的PBH双星在其GW进入除LISA之外的任何GW频段时会完全圆化，而在LISA频段可能存在$O(10^{-2})$量级的残余偏心率。成为暗物质晕一部分的双星可能会与其他PBH发生多次双星 - 单星相互作用，特别是如果它们位于更密集的环境中，即使在晚期吸积阶段也可能具有更高的偏心率，可被GW天文台探测到。考虑到目前对恒星质量范围内PBHs丰度的限制，我们预测LISA和DECIGO一起能够探测到$O(10^2)$个偏心率$e>0.01$的此类双星。如果这些未来的空间GW天文台能够排除此类偏心双星，那么PBH丰度的限制可以提高一个数量级。
英文摘要
Primordial black hole (PBH) binaries in the stellar mass range may still contribute a fraction of the detectable compact object binaries by LIGO and future GW observatories. PBH binaries at formation typically have very high eccentricities. In this paper, we study the eccentricity of stellar mass range PBH binaries from all formation channels and account for all evolutionary pathways. We simulate large samples of PBH binaries, tracking their full orbital evolution up to their merger or to the present day. For those that merge, we compute their GW strain, detectability, and eccentricity distributions for LISA, DECIGO, ET, CE, and aLIGO. We find that PBH binaries that evolve in isolation completely circularize by the time their GWs enter any GW band except for LISA's, where residual eccentricities of order $O(10^{-2})$ can exist. Binaries that become part of dark matter halos can have multiple binary-single interactions with other PBHs, especially if they reside in the more dense environments among them and can have higher eccentricities even at their late inspiral phase, probed by the GW observatories. Considering the current limits on the abundance of stellar mass range PBHs, we predict that LISA and DECIGO together would be able to probe $O(10^2)$ such binaries with $e>0.01$. If these future GW observatories in space can exclude such eccentric binaries, then limits on the PBH abundance can be improved by an order of magnitude.
Comments14 pages,10 figures
