Big Bang nucleosynthesis

We make generic remarks about baryogenesis in models where the scale M s of quantum gravity is much below the Planck scale. These correspond to M-theory vacua with a large volume for the internal space. Baryogenesis is a challenge, particularly for M s Շ10 5 GeV, because there is an upper bound on the reheating temperature of the Universe, and because certain baryon number violating operators must be suppressed. We discuss these constraints for different values of M s , and illustrate with a toy model the possibility of using horizontal family symmetries to circumvent them. ͓S0556-2821͑99͒06410-3͔

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Primordial nucleosynthesis and finite temperature QED

Haseeb

Jan

Sarfaraz

2014

Int. J. Mod. Phys. D

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Abundances of light nuclei formed during primordial nucleosynthesis are predicted by Standard Big Bang Model. The latest data from WMAP, with precision's higher than ever before, provides a motivation to determine theoretical higher order corrections to change in helium abundance and the related parameters. Here we evaluate the QED corrections to the change in these parameters during primordial nucleosynthesis using finite temperature effects at the two loop level. Relative variations in neutron decay rate, total energy density of the universe, relative change in neutrino temperature etc., with two loop corrections to electron mass, at the timescale when QED corrections were relevant, have been estimated.

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Big Bang nucleosynthesis

Cited by 3 publications

References 32 publications

The role of 3He in nuclear astrophysics

The role of 3He in nuclear astrophysics

Baryogenesis in models with a low quantum gravity scale

Primordial nucleosynthesis and finite temperature QED

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