Quintom fields from chiral anisotropic cosmology

TL;DR

This paper investigates a chiral anisotropic cosmological model with quintom fields, providing classical solutions that include a big-bounce and isotropization, and quantum solutions showing damped probability densities and potential anisotropy vanishing.

Contribution

It introduces a novel analysis of quintom fields in chiral anisotropic cosmology, offering analytical classical and quantum solutions and insights into singularity resolution and isotropization.

Findings

Classical solutions include a big-bounce replacing the big bang.

Quantum probability density is damped and tends to flat FLRW as anisotropies vanish.

Quantum analysis suggests anisotropies diminish for certain parameter values.

Abstract

In this paper we present an analysis of a chiral anisotropic cosmological scenario from the perspective of quintom fields. In this setup quintessence and phantom fields interact in a non-standard (chiral) way within an anisotropic Bianchi type I background. We present our examination from two fronts: classical and quantum approaches. In the classical program we find analytical solutions given by a particular choice of the emerged relevant parameters. Remarkably, we present an explanation of the ''big-bang'' singularity by means of a ''big-bounce''. Moreover, isotropization is in fact reached as the time evolves. On the quantum counterpart the Wheeler-DeWitt equation is analytically solved for various instances given by the same parameter space from the classical study, and we also include the factor ordering $\rm Q$. Having solutions in this scheme we compute the probability density, which is in effect damped as the volume function and the scalar fields evolve; and it also tends towards a flat FLRW framework when the factor ordering constant $\rm Q \ll 0$. This result might indicate that for a fixed set of parameters, the anisotropies quantum-mechanically vanish for very small values of the parameter $\rm Q$. Finally, classical and quantum solutions reduce to their flat FLRW counterparts when the anisotropies vanish.