从夸克到宇宙：宇宙演化中的粒子与等离子体
Quarks to Cosmos: Particles and Plasma in Cosmological evolution
AI总结：
本文在粒子物理标准模型框架下，利用FLRW宇宙学描述130 GeV至20 keV温度范围内宇宙的演化，通过减速参数划分时期，分析粒子丰度变化、中微子脱耦及电子-正电子等离子体的屏蔽和顺磁效应。
摘要：
我们在粒子物理（PP）标准模型（SM）'PP-SM'的背景下，描述了温度范围$130\GeV>T>20\keV$内宇宙的原始性质与组成。宇宙演化采用FLRW宇宙学描述。我们呈现了跨时间粒子含量的全局视图，并使用减速参数$q$描述了不同的演化时期。我们沿着膨胀和冷却宇宙中的时间箭头前进：在PP-SM重粒子$(t, h, W, Z)$的丰度在$T\simeq 50\GeV$以下减少后，宇宙中的PP-SM等离子体由强相互作用的夸克-胶子成分主导。一旦温度降至$T\simeq 150\MeV$以下，夸克和胶子强子化为强相互作用物质粒子。重子反物质的迅速消失完成于$T_\mathrm{B}=38.2\MeV$。我们研究了随之而来的奇异性和介子整体的消失。我们表明，由粒子群体定义的不同时期彼此几乎不分离，μ子丰度恰在$T=\mathcal{O}(2.5)\MeV$之前消退，即自由流中微子出现的时期。我们讨论了控制中微子脱耦的两个相关基本常数。随后，我们跟随原始宇宙经历热致密电子-正电子等离子体时期。正电子反物质的高密度在$T=20.3\keV$附近消失：核反应发生在高度移动且相对强相互作用的电子-正电子等离子体相存在的情况下。我们应用等离子体理论方法描述重尘埃粒子（核子）之间的强屏蔽效应。我们分析了电子-正电子等离子体在暴露于外部原始磁场时的顺磁特性。
英文摘要：
We describe in the context of the particle physics (PP) standard model (SM) `PP-SM' the understanding of the primordial properties and composition of the Universe in the temperature range $130\GeV>T>20\keV$. The Universe evolution is described using FLRW cosmology. We present a global view on particle content across time and describe the different evolution eras using deceleration parameter $q$. We follow the arrow of time in the expanding and cooling Universe: After the PP-SM heavies $(t, h, W, Z)$ diminish in abundance below $T\simeq 50\GeV$, the PP-SM plasma in the Universe is governed by the strongly interacting Quark-Gluon content. Once the temperature drops below $T\simeq 150\MeV$, quarks and gluons hadronize into strongly interacting matter particles. Rapid disappearance of baryonic antimatter completes at $T_\mathrm{B}=38.2\MeV$. We study the ensuing disappearance of strangeness and mesons in general. We show that the different eras defined by particle populations are barely separated from each other with abundance of muons fading out just prior to $T=\mathcal{O}(2.5)\MeV$, the era of emergence of the free-streaming neutrinos. We discuss the two relevant fundamental constants controlling the decoupling of neutrinos. We subsequently follow the primordial Universe as it passes through the hot dense electron-positron plasma epoch. The high density of positron antimatter disappears near $T=20.3\keV$: Nuclear reactions occur in the presence of a highly mobile and relatively strongly interacting electron-positron plasma phase. We apply plasma theory methods to describe the strong screening effects between heavy dust particle (nucleons). We analyze the paramagnetic characteristics of the electron-positron plasma when exposed to an external primordial magnetic field.
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