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.

利用LIGO和VIRGO观测到的第一颗双中子星合并GW170817，引领科学界进入引力波多信使天文学时代。 数值相对论模拟表明，热致密物质的压力-密度关系（称为状态方程）在模拟中子星碰撞中发挥着基础作用。 中子星的质量是太阳的两倍，但直径通常只有 20 公里左右。在如此惊人的密度下，原子核会塌陷，中子和质子被紧紧地挤压在一起，以至于它们可能会分解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、最先进的超密核物质状态方程模型，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，并识别夸克可能在中子星合并产生的引力波信号中记录自己的可能信号。状态方程模型将通过在线服务（CompOSE、StellarCollapse）向社区提供。圣地亚哥州立大学的研究生和本科生将接受丰富的跨学科物理领域的培训，丰富他们在课堂上学到的教育经验。该项目的总体目标是确定一套全面的最先进的热致密核物质状态方程模型，供从事中子星合并模拟的研究人员使用。 当代有效场理论模型，即相对论密度依赖 Hartree (DDRMF) 模型和（局部和非局部）3 味 Polyakov-Nambu-Jona-Lasinio (3PNJL) 模型，将用于实现这一目标。 DDRMF 是一种多功能且易于数值处理的核多体理论，非常适合研究致密和致密强子物质。 3PNJL 模型是量子色动力学的有效模型，可以对夸克物质进行当代建模。它为量子色动力学提供了一种功能性且易于数值处理的方法。该模型解释了手性对称性的动态破缺，并通过波利亚科夫环势模拟夸克禁闭。将使用吉布斯和麦克斯韦相平衡条件来研究零温度和有限温度下的夸克解除限制。目前来自核理论、核实验和天体物理学的最强约束将用于确定有效场论的参数并测试状态方程的有效性。该项目推进了“宇宙之窗：多信使天体物理学时代”的目标，这是未来 NSF 投资的 10 大创意之一。该奖项反映了 NSF 的法定使命，并被认为值得通过以下方式获得支持： 使用基金会的智力价值和更广泛的影响审查标准进行评估。

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