A Complete Model of Cosmological Evolution of Scalar Field with Higgs Potential and Euclidian Cycles
arXiv:2005.14010 · doi:10.1134/S0202289320010065
Abstract
The revision of the Author's results with respect to possibility of existence of the so-called Euclidian cycles in cosmological evolution of a system of Higgs scalar fields has been performed. The assumption of non-negativity of the Universe's extension velocity, which contradicts in certain cases to complete system of Einstein equations, has been removed. It has been shown that in cases when effective energy of the system tends to zero, a smooth transition of the model to the range of negative values of the extension velocity occurs, i.e. it occurs the transition to collapse stage rather than winding of the phase trajectories on the boundary of prohibited area. This process has been researched with a help of numerical simulation methods for the model based on classical scalar Higgs field.
10 pages, 10 references, 12 figures
References in corpus (5)
- On the Null Energy Condition and Cosmology
- Cosmological Evolution of Statistical System of Scalar Charged Particles
- Exact Solutions for Nonlocal Nonlinear Field Equations in Cosmology
- Dynamics of cosmological models with nonlinear classical phantom scalar fields. II. Qualitative analysis and numerical modeling
- Dynamics of cosmological models with nonlinear classical phantom scalar fields. I. Formulation of the mathematical model
Cited by in corpus (7)
- Complete cosmological model based on a asymmetric scalar Higgs doublet
- Cosmological Models Based on a Statistical System of Scalar Charged Degenerate Fermions and an Asymmetric Higgs Scalar Doublet
- Cosmological evolution of a statistical system of degenerate scalar-charged fermions with an asymmetric scalar doublet. I. Two-component system of assorted charges
- Evolution of plane perturbations in the cosmological environment of the Higgs scalar field and an ideal scalar charged fluid
- Stability of the cosmological system of degenerated scalar charged fermions and Higgs scalar fields. I. Mathematical model of linear plane perturbations
- Complete cosmological evolution model of a classical scalar field with a higgs potential. II. Numerical simulation
- Complete cosmological evolution model of a classical scalar field with a Higgs potential. III. Features of phase trajectory flows