Electroweak vacuum instability and renormalized Higgs field vacuum fluctuations in the inflationary universe

被引：15

作者：

Kohri, Kazunori ^{[1
,2
]}

Matsui, Hiroki ^{[2
]}

机构：

[1] KEK, Inst Particle & Nucl Studies, 1-1 Oho, Tsukuba, Ibaraki 3050801, Japan

[2] Grad Univ Adv Studies SOKENDAI, 1-1 Oho, Tsukuba, Ibaraki 3050801, Japan

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2017年 / 08期

关键词：

cosmology of theories beyond the SM; inflation; quantum cosmology; physics of the early universe; ENERGY-MOMENTUM TENSOR; BACK-REACTION PROBLEM; ADIABATIC REGULARIZATION; SCALAR FIELD; INTERACTING THEORIES; CURVED SPACETIME; FALSE VACUUM; FATE; METASTABILITY; PROPAGATOR;

D O I：

10.1088/1475-7516/2017/08/011

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In this work, we investigated the electroweak vacuum instability during or after inflation. In the inflationary Universe, i. e., de Sitter space, the vacuum field fluctuations <delta phi(2)> enlarge in proportion to the Hubble scale H-2. Therefore, the large inflationary vacuum fluctuations of the Higgs field <delta phi(2)> are potentially catastrophic to trigger the vacuum transition to the negative-energy Planck-scale vacuum state and cause an immediate collapse of the Universe. However, the vacuum field fluctuations <delta phi(2)> i.e., the vacuum expectation values have an ultraviolet divergence, and therefore a renormalization is necessary to estimate the physical e ff ects of the vacuum transition. Thus, in this paper, we revisit the electroweak vacuum instability from the perspective of quantum fi eld theory (QFT) in curved spacetime, and discuss the dynamical behavior of the homogeneous Higgs field phi determined by the effective potential V-eff (phi) in curved space-time and the renormalized vacuum fluctuations <delta phi(2)>(ren) via adiabatic regularization and point-splitting regularization. We simply suppose that the Higgs fi eld only couples the gravity via the non-minimal Higgs-gravity coupling xi(mu). In this scenario, the electroweak vacuum stability is inevitably threatened by the dynamical behavior of the homogeneous Higgs field phi, or the formations of AdS domains or bubbles unless the Hubble scale is small enough H < Lambda(I).

引用

页数：26

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