夸克-强子方法模拟混合星
Modeling Hybrid Stars in Quark-Hadron Approaches
摘要：
对中子星或更一般的致密星的研究，是核天体物理学中的一个中心课题。此外，中子星是唯一的物理系统，其性质可以用来推断几倍于核饱和密度的冷而致密的物质的信息。因此，中子星物理学非常适合补充超相对论性重离子碰撞的研究，这些碰撞在高温和相对较小的净重子密度下对强相互作用物质进行采样。一般来说，为了确定或至少限制致密物质的性质，需要精确测量中子星的性质，如质量、半径、旋转频率和冷却行为。在这里，在相对较近的时间，可靠的质量测定脉冲星PSR J1614-2230的$M = 1.97 \pm 0.04 M_\odot$介绍了一个重要的基准建模恒星和强相互作用的物质。它对致密恒星的结构和恒星核心可能的奇异相位施加了限制，这将在本文中讨论。为了研究这一点，我们将考虑一个模型的恒星物质，其中包括超子和夸克自由度，并目前的结果，紧凑的恒星性质在下面。
英文摘要：
The study of neutron stars, or more general compact stars, is a topic of central interest in nuclear astrophysics. Furthermore, neutron stars serve as the only physical systems whose properties can be used to infer information on cold and dense matter at several times nuclear saturation density. Therefore, neutron star physics is ideally suited to complement the studies of ultra-relativistic heavy-ion collisions that sample strongly interacting matter at high temperature and relatively small net baryon density. In general, in order to pin down or at least constrain the properties of dense matter, accurate measurements of neutron star properties like masses, radii, rotational frequency, and cooling behavior are needed. Here, in relatively recent times the reliable mass determination of the pulsar PSR J1614-2230 of $M = 1.97 \pm 0.04 M_\odot$ has introduced an important benchmark for modeling stars and strongly interacting matter. It puts constraints on the structure of compact stars and possible exotic phases in the core of the stars as will be discussed in this article. In order to investigate this point we will consider a model for star matter that includes hyperonic and quark degrees of freedom, and present results for compact star properties in the following.
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