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arXiv · 1702.04630

Inflationary Cosmology in Scalar-Tensor Gravity: Reconstructing Higgs-Like Potentials

Anderson Mendonça da Silva·Jim E. F. Skea
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Abstract

We study cosmology in scalar-tensor (Bergmann Wagoner) gravity, restricting the coupling function, ${\omega}({\phi})$ to be constant. Rather than specify the form of the cosmological function, ${\lambda}({\phi})$, the scalar field is modelled as a function which decays to its present value ${\phi}=1$. Solutions of the field equations are found for which ${\lambda}({\phi})$ evolves from a large value (approximately 1) near the singularity to a small, non-zero value at later times, avoiding the problem of pre-inflationary collapse in standard general relativistic cosmology. Interpreting the model within the framework of Brans-Dicke theory with a scalar potential, we find that for suitable initial conditions, the reconstructed potential at late times for flat, open and closed universes is well described by a Higgs-like Mexican hat potential, quartic in ${\phi}$, though this was not built in to the initial assumptions.

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Anderson Mendonça da Silva, Jim E. F. Skea. 2017-02-14. Inflationary Cosmology in Scalar-Tensor Gravity: Reconstructing Higgs-Like Potentials. https://arxiv.org/abs/1702.04630

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