NEUTRINO MASSES AND THE BARYON ASYMMETRY

By W. Buchmuller, M. Plumacher. 2000

173 citations recorded by the source corpus.

Due to sphaleron processes in the high-temperature symmetric phase of the standard model the cosmological baryon asymmetry is related to neutrino properties. For hierarchical neutrino masses, with B-L broken at the unification scale ΛGUT~1016 GeV, the observed baryon asymmetry nB/s~10-10 can be naturally explained by the decay of heavy Majorana neutrinos. We illustrate this mechanism with two models of neutrino masses, consistent with the solar and atmospheric neutrino anomalies, which are based on the two symmetry groups SU(5)×U(1)F and SU(3)c×SU(3)L×SU(3)R×U(1)F. We also review related cosmological bounds on Majorana neutrino masses and the use of Boltzmann equations.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/9ce038faf9e3f3692fcfc9e4c4cc727c0c8e0118

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

Cosmological bounds on neutrino degeneracy improved by flavor oscillations (2002, background): “While B − L = 0 is motivated by scenarios where the baryon asymmetry is obtained via leptogenesis [1], there are models for producing large L and small B [2–5].”
Thermal production of gravitinos (2000, background): “In models of baryogenesis where the cosmological baryon asymmetry is generated in heavy Majorana neutrino decays [17], temperatures TR ≃ 108 − 1010 GeV are of particular interest [ 18 ].”
A facility to search for hidden particles at the CERN SPS: the SHiP physics case (2015, methodology): “[643, 653]), type II [370, 654, 655], and type III [656, 657] seesaws, mostly using Boltzmann Equations as pioneered by [658].”
Type II leptogenesis and the neutrino mass scale (2004, background): “In the effective approach and for thermal leptogenesis with a reheating temperature TR ≫ MR1, which is most independent of the cosmological model and of the model for neutrino masses, we assume that to a good approximation the efficiency factor depends only on the quantity m̃1 [22], defined by”
Dark energy from mass varying neutrinos (2003, unknown): “[78–85].”
Running neutrino masses, mixings and CP phases: Analytical results and phenomenological consequences (2003, background): “As a detailed numerical calculation of the dilution factor is beyond the scope of this paper, we refer to [45], from which we see that in the region of interest, i.”
Leptogenesis (2008, unknown): “Various reviews [57, 58] were written at this stage, a pedagogical presentation that introduces BE, and discusses models and supersymmetry can be found in [58].”