强子-夸克混合相状态方程的天体物理意义：致密星和恒星坍缩
Astrophysical Implications of Equation of State for Hadron-Quark Mixed Phase: Compact Stars and Stellar Collapses
摘要：
我们构造了一个包含强子-夸克相变的状态方程。混合相是由有限温度下的吉布斯条件得到的。我们采用基于相对论平均场论的状态方程来描述考虑π介子的强子相。对于夸克相，我们采用了量子化的三味奇异夸克物质的MIT袋模型。因此，我们的状态方程是热力学稳定的，定性地表现出强子-夸克混合物质所需的性质，如跃迁密度的温度依赖性。π介子提高了跃迁密度，因为它们使物态方程变软了。利用本文建立的状态方程，我们研究了它的天体物理意义。研究了致密星的最大质量，我们的状态方程与最近的观测结果一致。我们还计算了一个质量为100个太阳质量的大质量恒星的坍缩，发现对于有π介子和夸克的模型，从反弹到黑洞形成的时间间隔变短。π介子和夸克影响了中微子的总能量，因为中微子发射的持续时间变短了。由于原中子星的密度变高，在π介子的作用下，中微子的光度也随之升高。
英文摘要：
We construct an equation of state including the hadron-quark phase transition. The mixed phase is obtained by the Gibbs conditions for finite temperature. We adopt the equation of state based on the relativistic mean field theory for the hadronic phase taking into account pions. As for the quark phase, the MIT bag model of the deconfined 3-flavor strange quark matter is used. As a result, our equation of state is thermodynamically stable and exhibits qualitatively the desired properties of hadron-quark mixed matter, such as the temperature dependence of the transition density. The pions raise the transition density because they make the equation of state softer. Using the equation of state constructed here, we study its astrophysical implications. The maximum mass of compact stars is investigated, and our equation of state is consistent with recent observations. We also compute the collapse of a massive star with 100 solar masses using our equation of state and find that the interval time from the bounce to the black hole formation becomes shorter for the model with pions and quarks. The pions and quarks affect the total energy of the emitted neutrinos because the duration time of the neutrino emission becomes shorter. The neutrino luminosity rises under the effect of pions since the density of the proto-neutron star becomes high.
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