Resolving the Peak of the Black Hole Mass Spectrum
Resolving the Peak of the Black Hole Mass Spectrum
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DOI：
10.3847/1538-4357/ac8b83
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发表时间：
2022-07
期刊：
影响因子：
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通讯作者：
E. Farag;M. Renzo;R. Farmer;Morgan T. Chidester;F. Timmes
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文献类型：
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作者：
E. Farag;M. Renzo;R. Farmer;Morgan T. Chidester;F. Timmes
引力波（GW）探测双星黑洞（BH）合并已经开始采样宇宙BH质量分布。单个恒星核心的演化预测了由于对不稳定超新星（PISNe）而导致的BH质量分布的差距。确定BH质量间隙的上边缘和下边缘对于解释GW对合并BH的检测可以是有用的。我们使用梅萨来演化单一的、非旋转的、金属丰度为Z = 10−5的大质量氦核，直到它们坍缩形成BH或爆炸为PISN，而不留下致密的残余物。我们计算了S（300 keV）=（77，203）keV B范围内S因子下BH质量能隙的边界，对应于我们的高分辨率表列12 C（α，γ）16 O反应速率概率分布函数中±3σ的不确定度。我们广泛地测试时间和空间分辨率，以解决BH质谱的理论峰穿过BH质量间隙。我们探讨了对流混合和核燃烧的收敛，发现需要显着的时间分辨率来实现收敛。我们还测试了采用最小扩散系数来帮助低分辨率模型达到收敛。根据12 C（α，γ）16 O速率的±3σ不确定度，我们建立了一个新的上质量能隙的下边缘为M下<$60 −14+32 M <$。我们研究了更大的3α速率对上质量隙下边缘的影响，发现M较低为<$69 −18+34 M <$。我们将我们的结果与引力波瞬态目录中报道的黑洞进行比较。
Gravitational-wave (GW) detections of binary black hole (BH) mergers have begun to sample the cosmic BH mass distribution. The evolution of single stellar cores predicts a gap in the BH mass distribution due to pair-instability supernovae (PISNe). Determining the upper and lower edges of the BH mass gap can be useful for interpreting GW detections of merging BHs. We use MESA to evolve single, nonrotating, massive helium cores with a metallicity of Z = 10−5, until they either collapse to form a BH or explode as a PISN, without leaving a compact remnant. We calculate the boundaries of the lower BH mass gap for S-factors in the range S(300 keV) = (77,203) keV b, corresponding to the ±3σ uncertainty in our high-resolution tabulated 12C(α,γ)16O reaction rate probability distribution function. We extensively test temporal and spatial resolutions for resolving the theoretical peak of the BH mass spectrum across the BH mass gap. We explore the convergence with respect to convective mixing and nuclear burning, finding that significant time resolution is needed to achieve convergence. We also test adopting a minimum diffusion coefficient to help lower-resolution models reach convergence. We establish a new lower edge of the upper mass gap as M lower ≃ 60−14+32 M ⊙ from the ±3σ uncertainty in the 12C(α, γ)16O rate. We explore the effect of a larger 3α rate on the lower edge of the upper mass gap, finding M lower ≃ 69−18+34 M ⊙. We compare our results with BHs reported in the Gravitational-Wave Transient Catalog.