We simulate numerically the formation of spherically symmetric primordial black holes (PBHs) seeded by different families of primordial curvature perturbations profiles in a radiation dominated Friedman-Robertson-Walker (FRW) Universe. We have studied the dependency on the curvature profile of the initial mass M _BH,i of the PBHs at the time of apparent horizon formation t _AH, and the final mass M _BH,f after the accretion process, using an excision technique, comparing M _BH,i to previous analytical estimations obtained using a compensated PBHs model approach. The analytical estimations are in agreement with numerical results, except for large values of the initial perturbation amplitude, when the compensated model is less accurate. The masses M _BH,f and M _BH,i do not depend only on the shape around the compaction function peak, but on the full profile of the initial curvature perturbation. We also estimate the accretion effects, and for PBHs with masses relevant for the dark matter abundance, with a final mass equal to the horizon crossing mass, we find M _BH,f ≈ 3 M _BH,i.

我们数值模拟了在辐射主导的弗里德曼-罗伯逊-沃克 (FRW) 宇宙中由不同族的原始曲率扰动分布所产生的球对称原始黑洞 (PBH) 的形成。我们已经研究了视层形成t _AH时 PBH的初始质量M _BH,i和吸积过程后的最终质量M _BH,f的曲率分布的依赖性，使用切除技术，比较了M _BH,i 使用补偿 PBH 模型方法获得的先前分析估计。解析估计与数值结果一致，除了初始扰动幅度的大值外，当补偿模型不太准确时。质量M _BH,f和M _BH,i不仅取决于压实函数峰值周围的形状_，还取决于初始曲率扰动的完整轮廓。我们还估计了吸积效应，对于质量与暗物质丰度相关的 PBH，最终质量等于地平线交叉质量，我们发现M _BH,f ≈ 3 M _BH,i。