On Effective Degrees of Freedom in the Early Universe

Abstract

We explore the effective degrees of freedom in the early universe, from before the electroweak scale at a few femtoseconds after the Big Bang, until the last positrons disappeared a few minutes later. We first look at the established concepts of effective degrees of freedom for energy density, pressure and entropy density, and introduce effective degrees of freedom for number density as well. We discuss what happens with particle species as their temperature cools down from relativistic to semi- and non-relativistic temperatures, and then annihilates completely. This will affect the pressure as well as the entropy per particle. We also look at the transition from a quark-gluon plasma to a hadron gas. Using a list of known hadrons, we use a "cross-over" temperature of 214 MeV where the effective degrees of freedom for a quark-gluon plasma equals that of a hadron gas.

29 pages, 7 figures

References in corpus (5)

• Observation of a new particle in the search for the Standard Model Higgs boson with the ATLAS detector at the LHC
• Observation of a new boson at a mass of 125 GeV with the CMS experiment at the LHC
• Relic neutrino decoupling with flavour oscillations revisited
• Neutrino mass from Cosmology
• Viscosity in a Lepton-Photon Universe

Cited by in corpus (2)

• Isocurvature bounds on axion-like particle dark matter in the post-inflationary scenario
• Entropy Production in a Lepton-Photon Universe