Search arXiv⌕ Search
Home/Archive/arXiv

arXiv · 2501.15597

Higgs Inflation Model with Small Non-Minimal Coupling Constant

Alexander B. Kaganovich
View original source ↗Read source document ↗Export metadata ↓

Abstract

The Higgs sector of the Two-Measure Theory (TMT) extension of the electroweak SM (TMSM) is studied in the context of cosmology, where the only non-zero component φ(t) of the cosmologically averaged Higgs field plays the role of the inflaton. The self-consistency of the system of equations has the form of an algebraic constraint defining the scalar ζequal to the ratio of two volume measures, as a function of φ. The ζis present in all equations of motion and has a significant effect on the dynamics. After the transition in the equations of motion to the Einstein frame, the resulting system of equations is described by the TMT-effective action S_{eff} and Lagrangian L_{eff}. Due to the constraint, the original model parameters are converted into φ-dependent classical effective parameters. The effective potential is U_{eff}=\frac{λ{4ξ^2}M_P^4\cdotF(φ)\cdot\tanh^4\bigl(\frac{\sqrtξφ}{M_P}\bigr), where F(φ)\approx \frac{1}{2} for φ>\sqrt{6}M_P. If ξ=1/6, then to ensure agreement with CMB observational data, the Higgs field self-coupling model parameter λmust be \sim10^{-11}. After the end of inflation, the decrease of φleads to a change in the sign of the effective Higgs mass term, that leads to SSB. As φapproaches VEV, ζchanges in such a way that the TMT-effective λincreases by 10 orders of magnitude to the value in the GWS theory. Applying the model to the very beginning of the classical evolution of the Universe shows that cosmological dynamics can begin with a "pathological" and even phantom regime. However, if evolution begins with normal dynamics, then it proceeds only as inflation, and the problem of initial conditions for the onset of inflation does not arise. The fermion preheating model is described as a preliminary study of preheating after inflation.

Explore related subjects

gr-qc

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Alexander B. Kaganovich. 2026-01-30. Higgs Inflation Model with Small Non-Minimal Coupling Constant. https://arxiv.org/abs/2501.15597

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

An upper bound on the minimum orbital period of black holes

Previous research has focused on establishing lower bounds on the minimum orbital period of black holes. In this work, we explore the complementary question of whether an upper bound exists for the minimum orbital period of black holes. We investigate the minimum orbital periods of three types of black holes: Schwarzschild, Reissner-Nordström and Kerr-Newman black holes. We find that the minimum orbital period of these black holes is bounded by an upper limit $T_{min} \leqslant 6\sqrt{3}πM$, where $M$ is the black hole mass. Our results suggest that this upper bound on the minimum orbital period may be a general property in black hole spacetimes.

gr-qc↗
arXiv2026

Dirac Observables for Gowdy Cosmologies regular at the Big Bang

Gowdy cosmologies are exact, spatially inhomogeneous solutions of the vacuum Einstein equations which describe nonlinear gravitational waves coalescing at the Big Bang singularity. With toroidal spatial sections they provenly have the Asymptotic Velocity Domination property, in that close to the Big Bang dynamical spatial gradients fade out and the dynamics is governed by a Carroll-type gravity theory. Here we construct an infinite set of Dirac observables for Gowdy cosmologies, valid off-shell, strongly, and without gauge fixing. These observables stay regular at the Big Bang and can be matched to much simpler Dirac observables of the Carroll-type gravity theory. Conversely, in an adapted foliation there is a systematic anti-Newtonian expansion (in inverse powers of the reduced Newton constant) of the full Dirac observables whose leading terms are the Carroll ones. In particular, this provides an off-shell generalization of the Asymptotic Velocity Domination property.

gr-qc↗
arXiv2026

Global causality constraints in rotating scalar-tensor spacetimes

Modified gravity is often formulated as an effective field theory (EFT), where higher-order corrections parametrize departures from General Relativity. We argue that such corrections should be constrained by the global causal structure of curved spacetime, in addition to the usual flat-space requirements such as positivity and unitarity. We propose that within the domain of validity of the EFT, the onset of closed timelike curves should not happen in a parametrically more accessible region than in the corresponding GR background. We test this diagnostic in the quadratic k-essence sector of scalar-tensor gravity. For stationary and axisymmetric spacetimes, the invariant test for closed axial orbits is the sign of the azimuthal component of the metric \(g_{φφ}\). We supplement this test by requiring a local time function in the space of Killing vectors. We apply these conditions to quadratic k-essence on Kerr--(A)dS backgrounds, with and without scalar charge. The zero-charge branch is exact Kerr--(A)dS, and we treat the charged branch perturbatively in scalar charge and in Hartle--Thorne slow rotation. Expanding for small spin \(χ=a/(GM)\ll1\), frame dragging begins at \(\mathcal O(χ)\), while the quadrupolar backreaction relevant for circular closed timelike curves enters at second order in both rotation and charge. We find that, in the truncation used here, any occurrence of \(g_{φφ}<0\) also lies outside EFT control. A higher-order calculation or a fully nonlinear treatment is therefore needed. Finally, we discuss how quasinormal modes and black-hole echoes could probe such causal structure.

gr-qc↗