# Equation of State for Cosmological Matter at and beyond QCD and Electroweak Eras

## TL;DR

This paper calculates the thermodynamic properties of cosmological matter across a wide temperature range, including QCD and electroweak eras, revealing complex phase transitions and providing an equation of state for early universe modeling.

## Contribution

It extends previous calculations by incorporating additional degrees of freedom up to TeV-scale temperatures, and identifies multiple crossover phase transitions in the early universe.

## Key findings

- QCD and EW phase transitions are crossovers.
- Equation of state varies from linear to complex and back to linear.
- Provides a comprehensive EoS for early universe expansion modeling.

## Abstract

Various thermodynamic quantities for baryon-free matter are calculated by combining the most reliable non-perturbative and perturbative calculations, especially the most recent ones including as many quark flavors as possible. We extend these calculations by including other degrees of freedom (dof), such as photons, neutrinos, leptons, electroweak particles, and Higgs bosons, that allows us to consider the temperatures up to the TeV-scale. The calculations show that similar to QCD, the EW phase transition is also a crossover. We have found that while the equation of state for the hadronic matter is linear, $p/\rho\simeq 0.2$, the one for higher temperatures is rather complex; it exhibits two crossover-type phase transitions, corresponding to strong and EW matter. At even larger energy densities, the deduced EoS becomes linear again and close to ideal gas. The combined equation of state can be used for modeling the expansion of the Universe from very early times and through the EW and QCD era.