Thermo-Nuclear Fusionin Early Universe

• Best tested theory of Early Universe

• Baryon-to-photon ratio h_nB/ng only parameter

• Neutron decay-anti-decay equilibrium ends when T~1MeV, they decay until they are captured in deuterium

• Deuterium eventually form 3He, 4He, 7Li, etc

• Most of neutrons end up in 4He

• Astronomical observations may suffer from further chemical processing in stars

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