堆芯坍塌模拟的扩展状态方程
An extended equation of state for core-collapse simulations
摘要：
在恒星核心坍缩事件中，物质被加热并压缩到高于核物质饱和密度的密度。对于质量超过25个太阳质量的原始恒星，它们最终形成一个黑洞，在坍缩过程中达到的温度和密度是如此之高，以至于传统的电子、原子核和核子的描述已经不再合适。本文提出了一个改进的状态方程，它还包含了π介子和超子。它们在高温和高密度状态下变得丰富。我们研究了不同的约束这样一个状态方程，来自超声波数据和观测的中子星的性质。为了测试零温度的版本，我们进行了数值模拟的中子星与这些额外的粒子到黑洞的崩溃。我们讨论的热力学性质的热版本的状态方程内的额外的粒子的影响，我们表明，在有关的核心崩溃和黑洞形成的制度，压力，内能和声速的影响，介子和超子是不可忽略的。
英文摘要：
In stellar core-collapse events matter is heated and compressed to densities above nuclear matter saturation density. For progenitors stars with masses above about 25 solar masses, which eventually form a black hole, the temperatures and densities reached during the collapse are so high that a traditional description in terms of electrons, nuclei, and nucleons is no longer adequate. We present here an improved equation of state which contains in addition pions and hyperons. They become abundant in the high temperature and density regime. We study the different constraints on such an equation of state, coming from both hyperonic data and observations of neutron star properties. In order to test the zero-temperature versions, we perform numerical simulations of the collapse of a neutron star with such additional particles to a black hole. We discuss the influence of the additional particles on the thermodynamic properties within the hot versions of the equation of state and we show that in regimes relevant to core-collapse and black hole formation, the effects of pions and hyperons on pressure, internal energy and sound speed are not negligible.
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