Equations of State of Superdense Nuclear Matter for Use in Neutron Star Merger Simulations

用于中子星合并模拟的超密核物质状态方程

• 批准号: 2012152
• 负责人: Fridolin Weber
• 金额: $ 31.5万
• 依托单位: San Diego State University Foundation
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2020
• 资助国家: 美国
• 起止时间: 2020-08-15 至 2024-07-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=2012152&HistoricalAwards=false
• 关键词: Equations; State; Superdense; Nuclear; Matter

The observation of the first binary neutron star merger named GW170817 using LIGO and VIRGO led the scientific community into the era of multi-messenger astronomy with gravitational waves. Numerical relativity simulations have shown that the pressure-density relationship (known as equation of state) of hot and dense matter plays a fundamental role in simulating the collisions of neutron stars. Neutron stars are up to twice as massive as our Sun but are typically only around 20 kilometers across. At such extraordinary densities, atomic nuclei collapse, and neutrons and protons are squeezed so tightly together that they may disintegrate into a plasma made of up and down quarks, which are the most fundamental building blocks of matter. The goal of this project is to determine a comprehensive set of state-of-the art models for the equation of state of superdense nuclear matter for use by researchers working on neutron-star merger simulations. In particular, the group will investigate the role of quarks for neutron-star mergers and identify possible signals by means of which quarks may register themselves in the gravitational-wave signals produced by merging neutron stars. The models for the equation of state will be made available to the community at online services (CompOSE, StellarCollapse). Graduate and undergraduate students at San Diego State University will be trained in areas of physics which are richly interdisciplinary and enrich their educational experience beyond what they learn in the classroom.The overarching goal of this project is to determine a comprehensive set of state-of-the art models for the equation of state of hot and dense nuclear matter for use by researchers working on neutron-star merger simulations. Contemporary effective field theoretical models, i.e., the relativistic density-dependent Hartree (DDRMF) model and the (local and the non-local) 3-flavor Polyakov-Nambu-Jona-Lasinio (3PNJL) model, will be used to accomplish this goal. The DDRMF is a versatile and numerically tractable nuclear many-body theory well suited for studies of dense and dense hadronic matter. The 3PNJL model is an effective model of quantum chromodynamics which allows for a contemporary modeling of quark matter. It provides a functional and numerically tractable approach to quantum chromodynamics. The model accounts for the dynamical breaking of chiral symmetry and mimics quark confinement via the Polyakov-loop potential. Quark deconfinement at zero and finite temperature will be studied using both the Gibbs and Maxwell condition for phase equilibrium. The strongest, currently possible constraints from nuclear theory, nuclear experiment, and astrophysics will be used to fix the parameters of the effective field theories and test the validity of the equations of state.This project advances the objectives of "Windows on the Universe: the Era of Multi-Messenger Astrophysics", one of the 10 Big Ideas for Future NSF Investments.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.

使用LIGO和VIRGO观测到的第一颗名为GW 170817的中子星星合并，将科学界带入了引力波多信使天文学的时代。 数值相对论模拟表明，热而致密物质的压力-密度关系（称为状态方程）在模拟中子星碰撞中起着重要作用。 中子星的质量是太阳的两倍，但通常只有20公里左右。在如此高的密度下，原子核会坍缩，中子和质子会被挤压得如此之紧，以至于它们可能会分裂成由上夸克和下夸克组成的等离子体，而上夸克和下夸克是物质最基本的组成部分。 该项目的目标是确定一套全面的超致密核物质状态方程最先进的模型，供从事中子星合并模拟的研究人员使用。特别是，该小组将研究夸克在中子星合并中的作用，并确定夸克可能在合并中子星产生的引力波信号中记录自己的可能信号。状态方程的模型将通过在线服务（CompOSE，StellarCollapse）提供给社区。圣地亚哥州立大学的研究生和本科生将接受物理学领域的培训，这些领域具有丰富的跨学科性，并丰富他们在课堂上学习之外的教育经验。该项目的总体目标是确定一套全面的最先进的模型，用于研究中子星合并模拟的研究人员使用的热而致密的核物质的状态方程。 现代有效场理论模型，即，相对论性密度依赖Hartree（DDRMF）模型和（局部和非局部）3味Polyakov-Nambu-Jona-Lasinio（3 PNJL）模型将用于实现该目标。DDRMF是一个通用的和数值上易于处理的核多体理论，非常适合于研究稠密和稠密强子物质。3 PNJL模型是一个有效的量子色动力学模型，它允许夸克物质的当代建模。它为量子色动力学提供了一种泛函的、数值上易于处理的方法。该模型考虑了手征对称性的动力学破缺，并通过Polyakov圈势模拟夸克禁闭。夸克解除禁闭在零和有限的温度将使用吉布斯和麦克斯韦相平衡条件进行研究。将利用核理论、核实验和天体物理学目前可能的最强约束来确定有效场论的参数，并检验状态方程的有效性。多信使天体物理学时代”，未来NSF投资的十大创意之一。该奖项反映了NSF的法定使命，并通过使用基金会的知识价值和更广泛的影响审查标准进行评估，被认为值得支持。

项目成果

Gravitational-Wave Instabilities in Rotating Compact Stars

旋转致密恒星中的引力波不稳定性

• DOI: 10.3390/galaxies10050094
• 发表时间: 2022
• 期刊: Galaxies
• 影响因子: 2.5
• 作者: Bratton, Eric L.;Lin, Zikun;Weber, Fridolin;Orsaria, Milva G.;Ranea-Sandoval, Ignacio F.;Saavedra, Nathaniel
• 通讯作者: Saavedra, Nathaniel

Fast-spinning and highly magnetized white dwarfs

快速旋转且高度磁化的白矮星

• 发表时间: 2021
• 期刊: World Scientific series in astrophysics
• 作者: Otoniel, E;Coelho, J;Malheiro, M;Weber, F.
• 通讯作者: Weber, F.

Constraints from compact star observations on non-Newtonian gravity in strange stars based on a density dependent quark mass model

基于密度依赖夸克质量模型的致密星观测对奇异星非牛顿引力的约束

• DOI: 10.1103/physrevd.103.043012
• 发表时间: 2021-01
• 期刊: PHYSICAL REVIEW D
• 影响因子: 5
• 作者: Shu-Hua Yang;Chun-Mei Pi;Xiao-Ping Zheng;Fridolin Weber
• 通讯作者: Fridolin Weber

Proto-Neutron Star Matter

原中子星物质

• DOI: 10.1088/1742-6596/2340/1/012013
• 发表时间: 2022
• 期刊: Journal of Physics: Conference Series
• 作者: Alp, A;Farrell, D;Weber, F;Malfatti, G;Orsaria, M G;Ranea-Sandoval, I F
• 通讯作者: Ranea-Sandoval, I F

Delta baryons and diquark formation in the cores of neutron stars

• DOI: 10.1103/physrevd.102.063008
• 发表时间: 2020-08
• 期刊: Physical Review D
• 影响因子: 5
• 作者: G. Malfatti;M. Orsaria;I. F. Ranea-Sandoval;G. Contrera;F. Weber