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arXiv 1612.08992nucl-thastro-ph.HE
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天体物理模拟中的广义密度泛函状态方程与三体力和夸克-胶子等离子体

Generalized density functional equation of state for astrophysical simulations with 3-body forces and quark gluon plasma

J. Pocahontas Olson, MacKenzie Warren, Matthew Meixner, Grant J. Mathews, N. Q. Lan, H. E. Dalhed

备注：
Submitted to Physical Review C. arXiv admin note: substantial text overlap with arXiv:1303.0064
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摘要：

本文提出了一个更新的通用核物质状态方程（EoS），用于模拟核心坍缩超新星、中子星合并和黑洞坍缩。这EoS制定的密度泛函理论（DFT）的背景下，并推广到包括所有DFT EoS符合已知的核和天体物理约束。该EoS还允许形成具有净质子过剩（$Y_p > 0.5$）的材料的可能性，并且具有对核统计平衡的改进的处理以及当密度接近核物质密度时向重核的过渡。我们包括了在核物质密度以上的范围内π介子的效应，并包括了所有已知的高温介子和重子态。我们分析了如何在密度泛函理论中的三体核力项在高密度下加强EoS以满足最大中子星约束，然而，对称性无能和π介子在高温下的形成的密度依赖性允许在超新星坍缩计算中软化中心核心，从而导致强大的爆炸。我们还增加了在核物质密度以上的量子色动力学手征对称性恢复和解除禁闭阶段的过渡的可能性。本文详细介绍了物理，和约束条件，这个新的EoS，并提出了一个说明，它的实施在中子星和核心坍缩超新星模拟。我们提出的核心坍缩超新星模拟与EoS的第一个结果。

英文摘要：

We present an updated general purpose nuclear equation of state (EoS) for use in simulations of core-collapse supernovae, neutron star mergers and black hole collapse. This EoS is formulated in the context of Density Functional Theory (DFT) and is generalized to include all DFT EoSs consistent with known nuclear and astrophysical constraints. This EoS also allows for the possibility of the formation of material with a net proton excess ($Y_p > 0.5$) and has an improved treatment of the nuclear statistical equilibrium and the transition to heavy nuclei as the density approaches nuclear matter density. We include the effects of pions in the regime above nuclear matter density and incorporate all of the known mesonic and baryonic states at high temperature. We analyze how a 3-body nuclear force term in the DFT at high densities stiffens the EoS to satisfy the maximum neutron star constraint, however the density dependence of the symmetry anergy and the formation of pions at high temperatures allows for a softening of the central core in supernova collapse calculations leading to a robust explosion. We also add the possibility of a transition to a QCD chiral-symmetry-restoration and deconfinement phase at densities above nuclear matter density. This paper details the physics, and constraints on, this new EoS and presents an illustration of its implementation in both neutron stars and core-collapse supernova simulations. We present the first results from core-collapse supernova simulations with this EoS.

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