arXiv 1902.055602019-02-14hep-phastro-ph.COgr-qchep-th

热背景中的Higgs畴壁

Higgs domain walls in the thermal background

Tomasz Krajewski, Zygmunt Lalak, Marek Lewicki, Paweł Olszewski

DOI：: 10.1016/j.dark.2019.100347

摘要：

大多数宇宙学模型预测宇宙在其演化的早期阶段是热的和致密的。本文分析了标准模型粒子热浴对宇宙学Higgs畴壁动力学的影响。这份手稿构成了我们早期工作的一个~扩展，在该工作中，我们研究了希格斯畴壁网络的演化，忽略了温度变化的影响。利用标准模型的热修正有效势，我们发现局域极大值$h_{max}$的位置和畴壁的宽度都强烈地依赖于温度$T$。对于高于$10^{10}\; \textrm{GeV}$的温度，它们分别与温度的增加成比例地增加和成反比地减少。因此，问题的能量尺度遵循温度的值。我们的数值晶格模拟的基础上的PRS算法显示，希格斯畴壁的存在下，背景热浴是非常不稳定的，并在形成后不久衰减。此外，我们还发现，为了使畴壁~网络的演化在电弱真空中结束，由Higgs场期望值高于$h_{max}$的暴胀产生的视界的分数需要很低。这意味着希格斯畴壁必然是非常罕见的物体，它们的平均能量密度非常小。因此，畴壁不能显著影响宇宙学观测值。

英文摘要：

Most cosmological models predict that the universe was hot and dense at the early stages of it's evolution. In this paper we analyse the influence of the thermal bath of Standard Model particles on the dynamics of cosmological Higgs domain walls. This manuscript poses an~extension of our earlier work in which we investigated the evolution of networks of Higgs domain walls neglecting the impact of temperature variation. Using the thermally corrected effective potential of Standard Model we have found that both the position of the local maximum $h_{max}$ separating minima and the width of domain walls strongly depend on temperature $T$. For temperatures higher than $10^{10}\; \textrm{GeV}$ they respectively increase proportionally and decrease inverse proportionally to the increasing temperature. Thus, the energy scale of the problem follows the value of temperature. Our numerical lattice simulations based on the PRS algorithm reveal that Higgs domain walls in the presence of the background thermal bath are highly unstable and decay shortly after formation. Moreover we have found that the fraction of horizons produced by inflation in which Higgs field expectation value is higher then $h_{max}$ needs to be very low in order for the evolution of the~network of the domain walls to end in the electroweak vacuum. This means that Higgs domain walls necessarily were very rare objects and their average energy density was very small. As a result, the domain walls can not significantly effect cosmological observables.

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