nLab QCD cosmology

Contents

matter field fermions (spinors, Dirac fields)

flavors of fundamental fermions in the standard model of particle physics:
generation of fermions	1st generation	2nd generation	3d generation
quarks ( $q$ )
up-type	up quark ( $u$ )	charm quark ( $c$ )	top quark ( $t$ )
down-type	down quark ( $d$ )	strange quark ( $s$ )	bottom quark ( $b$ )
leptons
charged	electron	muon	tauon
neutral	electron neutrino	muon neutrino	tau neutrino

bound states:
mesons	light mesons: pion ( $u d$ ) ρ-meson ( $u d$ ) ω-meson ( $u d$ ) f1-meson a1-meson	strange-mesons: ϕ-meson ( $s \bar s$ ), kaon, K-meson ( $u s$ , $d s$ ) eta-meson ( $u u + d d + s s$ ) charmed heavy mesons*: D-meson ( $u c$ , $d c$ , $s c$ ) J/ψ-meson ( $c \bar c$ )	bottom heavy mesons: B-meson ( $q b$ ) ϒ-meson ( $b \bar b$ )
baryons	nucleons: proton $(u u d)$ neutron $(u d d)$

hadrons (bound states of the above quarks)

bosinos:

dark matter candidates

Exotica

auxiliary fields

Idea

The evolution of the early observable universe must have been crucially affected by the properties (e.g. equation of state) of the primordial quark-gluon plasma, and then, as the temperature decreased, by its confinement phase transition during nucleosynthesis to a hadron gas?. The study of the properties of QCD relevant for cosmology this way is called QCD cosmology.

The crucial effects in QCD cosmology are thus controlled by quantum chromodynamics (QCD) and specifically in its non-perturbative confined phase, hence are subject to the confinement problem.

Paolo Castorina, Vincenzo Greco, Salvatore Plumari, QCD Equation of State and Cosmological Parameters in Early Universe, Phys. Rev. D 92, 063530 (2015) (arXiv:1505.07655)

Michael McGuigan, Wolfgang Söldner, QCD Cosmology from the Lattice Equation of State (arXiv:0810.0265)
Sz. Borsanyi et al. Lattice QCD for Cosmology (arXiv:1606.07494)

Last revised on April 10, 2020 at 15:35:57. See the history of this page for a list of all contributions to it.