EW & QCD Phase Transition in the Early Universe and the Structure of Vacuum

在1994年和1995年的头两年，我们构建了研究宇宙一阶相变的理论框架。这包括两个部分。首先描述了强子泡在相变过冷期的形核及其生长过程，其次描述了宇宙重新加热到临界温度后重子数通过相界转移的过程。此外，我们在1996年建立了适用于有限温度和密度真空的量子色动力(QCD)的有效唯象模型。我们考虑了最近格点规范模拟的所有理论成果，它们可以描述手征对称性自发破缺和色约束，我们将这些理论模型相互结合起来，尝试求解重子数…随时间变化的积分-微分方程组数值计算表明，高温QGP相和低温强子相中的BER密度较大。我们使用NAO的大型计算机和工作站来执行这个程序。然后我们发现，由一阶宇宙QCD相变最终产生的非均匀重子数密度具有很大的密度对比度，在T=1 MeV核合成时期，涨落之间的平均间隔距离从10米到视界尺度。这些涨落距离尺度强烈地依赖于基本的QCD参数。事实证明，重子非均匀宇宙学中的原始核合成与均匀大爆炸核合成有很大不同。最引人注目的结果是，我们的宇宙学模型可以允许非常大的宇宙平均重子密度，正如最近在富星系团或超星系团中的天文观测所表明的那样。我们将这些原始丰度应用到星系化学演化的研究中，并提出了几个天文观测，以检验我们的非均匀重子密度宇宙的宇宙学模型。较少

In the first two years 1994 and 1995 we constructed theoretical framework for the studies of cosmological first order phase transition. This consists of two parts. The first is to describe the nucleation of hardronic bubbles and their growth process during the supercooling epoch of the phase transition, and the second is to formulate the process of baryon number transfers through the phase boundary after the Universe was reheated to the critical temperature.In addition to these theoretical studies, we constructed in this year 1996 the effective phenomenological model Lagrangian for Quantum Chromodynamins (QCD) which is applied to the vacuum at finite temperature and density. We took account of all recent theoretical products from the lattice gauge simulations of which can describe spontaneous chiral symmetry breaking and also color confinement.We combined these theoretical models with one another and tried to solve the integro-differential equations for the time variation of baryon num … More ber densities in the high-temperature QGP phase and low-temperature hadron phase numerically. We used big computers and workstations at NAO in performing this program. We then found that the inhomoegenous baryon number densities which arises eventually from the first order cosmological QCD phase transition have very huge density contrast as large as a million or more and that the mean separation distance between the fluctuations ranges from ten meters to the horizon scale at T=1 MeV nucleosynthesis epoch. These fluctuation distance scales depend strongly on the fundamental QCD parameters. The primordial nucleosynthesis in the baryon inhomogeneous cosmology turns out to be dramatically different from the homogeneous big-bang nucleosynthesis. The most striking result is that our cosmological model can allow very large universal average baryon density, as was suggested from the recent astronomical observations in rich clusters or superclusters. We applied these primordial abundances to the studies of chemical evolution of galaxies and proposed several astronomical observations in order to test our cosmological model of inhomogeneous baryon density Universe. Less