论文标题
使用多中音恒定观察来限制中子恒星状态的方程
Constraining the equation of state of neutron stars using multimessenger observations
论文作者
论文摘要
中子恒星是我们可见宇宙中已知的最密集的物体。中子星内物质的特性在其状态方程中编码，从理论角度来看，它具有广泛的不确定性。有了当前对量子染色体动力学的理解，很难在如此高的密度下确定中子恒星物质的相互作用。同样，进行许多身体计算在计算上也很棘手。除了中子之星核心的构成外，还没有排除，它包含奇怪的baryons，介子冷凝水，夸克物质等奇特物质。尽管中子恒星内的物质非常稠密，但是该物体的温度在其大部分寿命中都非常寒冷。我们不能在我们的实验室中生产这种稠密而相当冷的材料。由于基于地球的实验无法探测中子恒星物质的物理学，因此我们寻找中子星的天体物理观察结果。该论文介绍了将中子星观测到从天体物理观察到其状态方程所需的理论和计算技术。
Neutron stars are the densest objects known in our visible universe. Properties of matter inside a neutron star are encoded in its equation of state, which has wide-ranging uncertainty from a theoretical perspective. With the current understanding of quantum chromodynamics, it is hard to determine the interactions of neutron star matter at such high densities. Also performing many body calculations is computationally intractable. Besides the constitution of the neutron star core is highly speculative -- it is not ruled out that it contains exotic matter like strange baryons, meson condensates, quark matter, etc. Although the matter inside the neutron star is extremely dense, but the temperature of this object is very cold in most of its life span. We cannot produce such dense but rather cold material in our laboratory. Since probing the physics of neutron star matter is inaccessible by our earth based experiments, we look for astrophysical observations of neutron stars. This thesis deals with the theoretical and computational techniques required to translate neutron star observables from astrophysical observations to its equation of state.
