RUI: Probing Quark Matter through Compact Star Oscillations

最近由NSF资助的美国LIGO天文台发现了黑洞引力波，这引起了公众的想象力，并为我们的宇宙打开了一扇新的观测窗口，就像伽利略时代望远镜的发现一样。科学界的广泛共识是，LIGO将很快探测到来自银河系众多中子星的引力波，这些中子星在20世纪60年代首次被无线电脉冲观测到。然而，与无线电波不同的是，引力波携带着关于中子星内部的信息，这将揭示高密度和高温度下核物理的新见解。该项目的重点是通过构建中子星及其发射信号的精确数学模型来提高探测中子星引力波的几率。PI将核物理学和天体物理学相结合，将使用现代计算算法来估计影响中子星发射的引力波光谱的关键参数。该研究的成果将减少寻找引力波信号的计算成本，完善现有的核物理模型，并培养CSU长滩的几名研究生的科学研究方法。在该项目中，PI将计算部分或全部由奇异夸克物质构成的致密恒星的非径向振荡模式，并研究它们与引力波特征的相关性。目标是发现模式谱中的趋势，这些趋势可以用作中子星内部结构的引力波指纹。利用流体动力学和广义相对论的理论原理，辅以数值程序，这项研究将促进对高密度核物理及其对致密星星振荡的影响的理解。这项研究的新方面包括调查组成梯度，超流性和混合相的夸克物质对多组分奇怪/混合星的振荡谱的影响。本研究所提出的方法涉及数值编码，以解决耦合方程的流体动力学在强引力时空内紧凑的恒星。通过这些任务，该项目将有助于量化现实夸克物质状态方程的非径向振荡模式，确定振荡谱的稳健和依赖模型的特征，并提出可由引力波探测器测试的中子星和奇异星之间的区别特征。

The recent discovery of gravitational waves from Black Holes by the NSF-funded US-based LIGO observatories has captured the public imagination and opened a new observational window to our Cosmos, much like the discovery of the telescope did in Galileo's time. There is broad consensus in the scientific community that LIGO will soon detect gravitational waves from numerous neutron stars in our Galaxy, which were first observed by radio pulses in the 1960s. Unlike radio waves however, gravitational waves carry information about the interior of neutron stars, which will reveal new insight into nuclear physics at high density and temperature. This project is focused on improving the odds of detecting the gravitational waves from neutron stars by constructing accurate mathematical models of neutron stars and the signals they emit. Integrating nuclear physics and astrophysics, the PI will use modern computational algorithms to estimate key parameters that affect the spectrum of gravitational waves emitted by neutron stars. Results from this research will reduce the computational cost of searching for gravitational wave signals, refine existing models of nuclear physics, and train several graduate students from CSU Long Beach in the methods of scientific research.In this project, the PI will calculate the non-radial oscillation modes of compact stars made in part or entirely of strange quark matter and will study their relevance to gravitational wave signatures. The goal is to discover trends in the mode spectrum that can be used as gravitational wave fingerprints of the inner structure of neutron stars. Using theoretical principles of fluid dynamics and general relativity, supplemented by numerical routines, this research will advance the understanding of nuclear physics at high density and its implications for compact star oscillations. Novel aspects of this research include investigating the impact of composition gradients, superfluidity, and mixed phases in quark matter on the oscillation spectrum of multi-component strange/hybrid stars. The proposed methods for this research involve numerical coding to solve coupled equations of fluid dynamics in strongly gravitating spacetime inside compact stars. Through these tasks, this project will help quantify the non-radial oscillation modes for realistic quark matter equations of state, identify robust and model-dependent features of the oscillation spectrum and propose distinguishing features between neutron stars and strange stars that can be tested by gravitational wave detectors.