论文标题
非本地夸克模型，用于描述中子星核中密集物质
Non-local quark models for description of dense matter in the cores of neutron stars
论文作者
论文摘要
这项论文的工作着重于研究核心塌陷超新星，中子星和描述了描述密集物质内部的理论模型的直接紧凑残留物中的相变的可能存在。具体而言，我们有兴趣分析这些物体内核中从辐射物质到夸克物质的过渡的可行性。对于相过渡，我们将使用两种不同的形式主义：麦克斯韦形式主义或突然的相变和吉布斯形式主义或混合相变。为了描述辐射物质，我们将使用具有密度依赖性耦合常数的相对论平均场模型的不同参数化。对于夸克物质的描述，我们将使用三种具有矢量相互作用的三种口味的有效的非局部nambu jona-lasinio模型，其中我们将包括形成diquarks的可能性，以建模$ su（3）$的颜色超导阶段。提出了在有限温度下的夸克物质状态的相图和方程，并研究了该类型物质对与中子恒星相关的观察物的影响。从原始恒星的状态到冷中子恒星的状态，研究了紧凑型恒星在其形成过程中的简化热演化，并将获得的结果与最近的天体物理观察结果进行了比较。获得的结果表明，这些恒星核中夸克物质的发生仍然是一种有希望的可能性。在这些对象中使用更逼真的模型来描述密集物质的事实表明，中子恒星中存在夸克物质，这可能是对这种物质行为的问题的答案，并确定了其相应的状态方程。
This thesis work focuses on studying the possible existence of phase transitions in the immediate compact remnants of core collapse supernova, neutron stars, and the theoretical models that describe the interior of dense matter. Specifically, we are interested in analyzing the feasibility of a transition from hadronic matter to quark matter in the cores of these objects. For the phase transition we will use two different formalisms: the Maxwell formalism or abrupt phase transition and the Gibbs formalisms or mixed phase transition. For the description of hadronic matter, we will use different parametrizations of the relativistic mean field model with density-dependent coupling constants. For the description of quark matter we will use an effective nonlocal Nambu Jona-Lasinio model of three flavors with vector interactions, in which we will include the possibility of formation of diquarks to model a superconducting phase of color in $SU(3)$. Phase diagrams and equations of state of quark matter at finite temperature are presented, and the influence of that type of matter on observables associated with neutron stars is investigated. The simplified thermal evolution of compact stars during their formation is studied, from their state of proto-neutron stars to that of cold neutron stars, and the results obtained are compared with recent astrophysical observations. The results obtained indicate that the occurrence of quark matter in the nuclei of these stars remains a promising possibility. The fact that the use of more realistic models for the description of the dense matter in these objects indicates the presence of quark matter inside neutron stars, could be an answer to the question of the behavior of that kind of matter and the determination of its corresponding equation of state.
