一个坍缩的超大质量恒星和黑洞形成的完全广义相对论中微子辐射-流体动力学模拟
A full general relativistic neutrino radiation-hydrodynamics simulation of a collapsing very massive star and the formation of a black hole
摘要：
我们研究了一个非常大质量的恒星的最终命运进行全面的广义相对论（GR），三维（3D）模拟与三味多能中微子输运。利用一个70太阳质量的零金属量的祖先，我们自洽地遵循辐射流体动力学从引力核坍缩的开始，直到第二次坍缩的原中子星（PNS），导致黑洞（BH）的形成。我们的研究结果表明，BH的形成发生在反弹后的时间为~300毫秒的70 Msun星。这明显早于文献中采用较低质量祖细胞的那些。在BH形成前几~10 ms，我们发现停滞的反弹冲击因来自非常热的PNS的强烈中微子加热而复活，这得益于冲击后面的剧烈对流。在3D-GR核心塌陷模型与多能量中微子输运的背景下，我们的数值计算结果提出了第一个证据，以验证一个回落BH形成的情况下，70 Msun星。
英文摘要：
We study the final fate of a very massive star by performing full general relativistic (GR), three-dimensional (3D) simulation with three-flavor multi-energy neutrino transport. Utilizing a 70 solar mass zero metallicity progenitor, we self-consistently follow the radiation-hydrodynamics from the onset of gravitational core-collapse until the second collapse of the proto-neutron star (PNS), leading to black hole (BH) formation. Our results show that the BH formation occurs at a post-bounce time of ~300 ms for the 70 Msun star. This is significantly earlier than those in the literature where lower mass progenitors were employed. At a few ~10 ms before BH formation, we find that the stalled bounce shock is revived by intense neutrino heating from the very hot PNS, which is aided by violent convection behind the shock. In the context of 3D-GR core-collapse modeling with multi-energy neutrino transport, our numerical results present the first evidence to validate a fallback BH formation scenario of the 70 Msun star.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
