Modeling the spectrum of gravitational waves in the primordial Universe

TL;DR

This paper explores how gravitational wave spectra can help distinguish dark energy models, specifically comparing generalized Chaplygin gas and $ ext{Lambda}$-CDM models, by analyzing their effects on the CMB.

Contribution

It introduces a massless gas component into the generalized Chaplygin gas model and compares the resulting gravitational wave spectra to previous models and $ ext{Lambda}$-CDM.

Findings

The new spectrum differs significantly from previous models.

Gravitational wave signatures can help differentiate dark energy models.

Comparison with $ ext{Lambda}$-CDM shows distinguishable features.

Abstract

Recent observations from type Ia Supernovae and from cosmic microwave background (CMB) anisotropies have revealed that most of the matter of the Universe interacts in a repulsive manner, composing the so-called dark energy constituent of the Universe. The analysis of cosmic gravitational waves (GW) represents, besides the CMB temperature and polarization anisotropies, an additional approach in the determination of parameters that may constrain the dark energy models and their consistence. In recent work, a generalized Chaplygin gas model was considered in a flat universe and the corresponding spectrum of gravitational waves was obtained. The present work adds a massless gas component to that model and the new spectrum is compared to the previous one. The Chaplygin gas is also used to simulate a $\Lambda$-CDM model by means of a particular combination of parameters so that the Chaplygin gas and the $\Lambda$-CDM models can be easily distinguished in the theoretical scenarios here established. The lack of direct observational data is partialy solved when the signature of the GW on the CMB spectra is determined.