nLab nucleosynthesis

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

Generally, nucleosynthesis refers to the formation of bound states of nucleons (protons and neutrons) to atomic nuclei. Specifically, primordial nucleosynthesis (often meant by default) is this process taking place in the early observable universe some comoving time after the big bang (see also at QCD cosmology). Other natural processes of nucleosynthesis happened and happen in stars? and in supernovae.

Dominik J. Schwarz, The first second of the Universe, Annalen Phys. 12:220-270, 2003 (arXiv:astro-ph/0303574)
Toshitaka Kajino, Cosmological Nucleosynthesis in the Big-Bang and Supernovae, Journal of Nuclear Science and Technology 39 sup2 (doi:10.1080/00223131.2002.10875156)
Grant J. Mathews, Motohiko Kusakabe, Toshitaka Kajino, Introduction to Big Bang Nucleosynthesis and Modern Cosmology, International Journal of Modern Physics EVol. 26, No. 08, 1741001 (2017) (arXiv:1706.03138, doi:10.1142/S0218301317410014)
James Alvey, What can you measure with BBN in 2021?, Cosmology Talks 2021 (pdf)