Comprehensive nucleosynthesis analysis for ejecta of compact binary mergers
Comprehensive nucleosynthesis analysis for ejecta of compact binary mergers
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DOI：
10.1093/mnras/stv009
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发表时间：
2015-03-21
影响因子：
4.8
通讯作者：
Janka, H-T
中科院分区：
文献类型：
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作者：
Just, O.;Bauswein, A.;Janka, H-T
我们提出了第一个全面的研究r-过程元素核合成的喷出物的紧凑的二元合并（CBM）和他们的遗迹黑洞（BH）-环面系统。的BH-吸积环面的演化模拟秒与牛顿流体动力学代码，包括粘性效应，伪牛顿引力的pseudo-Newtonian gravity for crackingBH，和一个依赖于能量的两个时刻封闭计划的电子中微子和反中微子的运输。所研究的情况是在相对论双中子星星（NS-NS）和NS-BH并合模型的指导下，产生了近似3-6个M圆点的BH，旋转参数A（BH）近似为0.8，环面为0.03-0.3个M圆点。我们的核合成分析包括动态（提示）喷出物在CBM阶段和中微子和粘性驱动流出的遗迹BH环面系统。虽然通常近似20%-25%的初始吸积环质量被粘性驱动的外流所损失，但中微子驱动的风最多贡献另一个近似1%，但中微子加热显着增强了粘性喷出物。由于BH-环面喷出物具有广泛的分布的电子分数（0.1-0.6）和熵，它们产生的重元素从A类似于80到锕系元素，与A大于或类似于130核的相对贡献是次优势和敏感地依赖于BH和环面质量和剪切粘度的确切处理。煤层气和BH-环面相的组合喷出物可以再现太阳丰度令人惊讶的是，大于或接近90。不同的贡献的环面喷出物可能会解释观察到的变化较轻的元素与40
We present the first comprehensive study of r-process element nucleosynthesis in the ejecta of compact binary mergers (CBMs) and their relic black hole (BH)-torus systems. The evolution of the BH-accretion tori is simulated for seconds with a Newtonian hydrodynamics code including viscosity effects, pseudo-Newtonian gravity for rotatingBHs, and an energy-dependent two-moment closure scheme for the transport of electron neutrinos and antineutrinos. The investigated cases are guided by relativistic double neutron star (NS-NS) and NS-BH merger models, producing similar to 3-6 M-circle dot BHs with rotation parameters of A(BH) similar to 0.8 and tori of 0.03-0.3 M-circle dot. Our nucleosynthesis analysis includes the dynamical (prompt) ejecta expelled during the CBM phase and the neutrino and viscously driven outflows of the relic BH-torus systems. While typically similar to 20-25 per cent of the initial accretion-torus mass are lost by viscously driven outflows, neutrino-powered winds contribute at most another similar to 1 per cent, but neutrino heating enhances the viscous ejecta significantly. Since BH-torus ejecta possess a wide distribution of electron fractions (0.1-0.6) and entropies, they produce heavy elements from A similar to 80 up to the actinides, with relative contributions of A greater than or similar to 130 nuclei being subdominant and sensitively dependent on BH and torus masses and the exact treatment of shear viscosity. The combined ejecta of CBM and BH-torus phases can reproduce the solar abundances amazingly well for A greater than or similar to 90. Varying contributions of the torus ejecta might account for observed variations of lighter elements with 40