Successful Common Envelope Ejection and Binary Neutron Star Formation in 3D Hydrodynamics.
Successful Common Envelope Ejection and Binary Neutron Star Formation in 3D Hydrodynamics.
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2020-11
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通讯作者：
J. Law-Smith;R. W. Everson;E. Ramirez-Ruiz;S. D. Mink;L. V. Son;Y. Gotberg;Stefan Zellmann;Alejandro Vigna-G'omez;M. Renzo;Samantha C. Wu;S. L. Schrøder;R. Foley;Tenley Hutchinson-Smith
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作者：
J. Law-Smith;R. W. Everson;E. Ramirez-Ruiz;S. D. Mink;L. V. Son;Y. Gotberg;Stefan Zellmann;Alejandro Vigna-G'omez;M. Renzo;Samantha C. Wu;S. L. Schrøder;R. Foley;Tenley Hutchinson-Smith
最近在引力波(GW)和电磁辐射(EM)的多信使探测中观察到了两颗中子星的合并。在哈勃时间内合并的双中子星，以及许多其他致密的双星，预计将通过共同的包络演化形成。然而，五十年来对共同包络演化的研究尚未导致对导致紧凑双星的系统的多空间多时间尺度演化的令人满意的理解。在这篇文章中，我们报道了首次在三维流体力学中成功地模拟了共同包络抛射导致双中子星的形成。在不同的初始分离和初始条件下，模拟了12$Modot红巨星与1.4美元Modot中子星相互作用的动力学激发相。在我们的所有模拟中，我们发现了完全的包络抛射和大约1.1美元-2.8R_ODOT$的最终轨道间隔，导致了一颗双星中子星将在0.01-1Gyr内合并。我们发现，对于我们研究的模型，其等价效率为$约0.1$-$0.4$，但这可能是这些扩展的前身所特有的。我们将恒星的核心完全分解为$\less sim 0.005 Rodot，我们的三维流体动力学模拟采用了调整后的一维解析能量公式和二维运动学研究，以克服模拟这些系统所需的高昂计算成本。我们在本文中开发的框架可以用来模拟恒星之间的各种相互作用，从恒星合并到导致GW源的常见包络事件。
The coalescence of two neutron stars was recently observed in a multi-messenger detection of gravitational wave (GW) and electromagnetic (EM) radiation. Binary neutron stars that merge within a Hubble time, as well as many other compact binaries, are expected to form via common envelope evolution. Yet five decades of research on common envelope evolution have not yet resulted in a satisfactory understanding of the multi-spatial multi-timescale evolution for the systems that lead to compact binaries. In this paper, we report on the first successful simulations of common envelope ejection leading to binary neutron star formation in 3D hydrodynamics. We simulate the dynamical inspiral phase of the interaction between a 12$M_\odot$ red supergiant and a 1.4$M_\odot$ neutron star for different initial separations and initial conditions. For all of our simulations, we find complete envelope ejection and a final orbital separation of $\approx 1.1$-$2.8 R_\odot$, leading to a binary neutron star that will merge within 0.01-1 Gyr. We find an $\alpha_{\rm CE}$-equivalent efficiency of $\approx 0.1$-$0.4$ for the models we study, but this may be specific for these extended progenitors. We fully resolve the core of the star to $\lesssim 0.005 R_\odot$ and our 3D hydrodynamics simulations are informed by an adjusted 1D analytic energy formalism and a 2D kinematics study in order to overcome the prohibitive computational cost of simulating these systems. The framework we develop in this paper can be used to simulate a wide variety of interactions between stars, from stellar mergers to common envelope episodes leading to GW sources.