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Hints for dynamical dark energy from warm inflation

Anupama B

Abstract

The effect of dissipation from the thermal bath of minimal warm inflation (MWI) on the temperature anisotropies of the cosmic microwave background (CMB) is investigated. A shift in the phase and peaks of the theoretical TT mode angular power spectrum of CMB for MWI with increasing dissipation strength hints at the dynamical nature of dark energy from warm inflation. Outcome of the study highlights the necessity of modifying the cosmological parameters, signalling a physics beyond the standard $Λ$CDM model of cosmology. The current findings may open a new direction for explaining the increased expansion rate in the early universe, thus alleviating some of the persistent tensions in cosmology, especially the Hubble tension.

Hints for dynamical dark energy from warm inflation

Abstract

The effect of dissipation from the thermal bath of minimal warm inflation (MWI) on the temperature anisotropies of the cosmic microwave background (CMB) is investigated. A shift in the phase and peaks of the theoretical TT mode angular power spectrum of CMB for MWI with increasing dissipation strength hints at the dynamical nature of dark energy from warm inflation. Outcome of the study highlights the necessity of modifying the cosmological parameters, signalling a physics beyond the standard CDM model of cosmology. The current findings may open a new direction for explaining the increased expansion rate in the early universe, thus alleviating some of the persistent tensions in cosmology, especially the Hubble tension.
Paper Structure (1 section, 3 equations, 1 figure)

This paper contains 1 section, 3 equations, 1 figure.

Table of Contents

  1. Acknowledgments

Figures (1)

  • Figure 1: The top left subfigure represents variation in the TT mode angular power spectrum of CMB with various allowed dissipation strength ($Q$) for MWI. The different regions marked in the main figure are shown separately in the remaining subfigures. Here, ($\Delta T_l )^2 = \frac{l(l+1)C_l }{2\pi}$ where $C_l$ the power spectrum of the multipole moments ($l$) of the temperature field.