夸克物质成核对原中子星演化的影响
Effects of quark matter nucleation on the evolution of proto-neutron stars
摘要：
在大质量中子星的核心中，存在着一种物质与非受限夸克强相互作用的相。如果这种解除禁闭的相变是第一级的，那么它将由亚稳强子相中的稳定夸克相的临界尺寸下降的成核所触发。在这些情况下，已经证明，冷纯强子致密星在其引力质量的阈值以上，相对于“衰变”到夸克星（致密星至少部分由夸克物质构成）是亚稳态的。这种恒星转换过程释放了大量的能量，它可能是一些长伽玛暴的能量来源。目前的工作的主要目标是确定一个新生的强子星（原强子星）是否可以生存的早期阶段的演变没有“衰变”的夸克星。为此，我们研究了热β稳定强子物质中夸克物质的成核过程，有和没有被捕获的中微子。我们计算和比较的成核速率和成核时间由于热和量子成核机制。我们计算的交叉温度以上的热成核占主导地位的有限温度量子成核机制。接下来我们讨论夸克物质成核对物理学和原中子星演化的影响。引入了原强子星极限转变温度和临界质量Mcr的新概念，证明了质量M <Mcr的原强子星可以在演化的早期阶段存活下来而不衰变为夸克星.我们扩展了“中子星“的最大质量的概念，相对于经典的一个由Oppenheimer & Schmidoff介绍的帐户存在两个不同的家庭的紧凑型恒星（强子星和夸克星）的预测目前的情况。
英文摘要：
(Abridged) A phase of strong interacting matter with deconfined quarks is expected in the core of massive neutron stars. If this deconfinement phase transition is of the first order then it will be triggered by the nucleation of a critical size drop of the stable quark phase in the metastable hadronic phase. Within these circumstances it has been shown that cold pure hadronic compact stars above a threshold value of their gravitational mass are metastable with respect to the "decay" to quark stars (compact stars made at least in part of quark matter). This stellar conversion process liberates a huge amount of energy, and it could be the energy source of some of the long GRBs. The main goal of the present work is to establish whether a newborn hadronic star (proto-hadronic star) could survive the early stages of its evolution without "decaying" to a quark star. To this aim, we study the nucleation process of quark matter in hot beta-stable hadronic matter, with and without trapped neutrinos. We calculate and compare the nucleation rate and the nucleation time due to thermal and quantum nucleation mechanisms. We compute the crossover temperature above which thermal nucleation dominates the finite temperature quantum nucleation mechanism. We next discuss the consequences of quark matter nucleation for the physics and the evolution of proto-neutron stars. We introduce the new concept of limiting conversion temperature and critical mass M_cr for proto-hadronic stars, and we show that proto-hadronic stars with a mass M < M_cr could survive the early stages of their evolution without decaying to a quark star. We extend the concept of maximum mass of a "neutron star" with respect to the classical one introduced by Oppenheimer & Volkoff to account for the existence of two distinct families of compact stars (hadronic stars and quark stars) as predicted by the present scenario.
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