The Neutrino Mass Window for Baryogenesis

By W. Buchmuller, P. Bari, M. Plümacher. 2003

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Interactions of heavy Majorana neutrinos in the thermal phase of the early universe may be the origin of the cosmological matter-antimatter asymmetry. This mechanism of baryogenesis implies stringent constraints on light and heavy Majorana neutrino masses. We derive an improved upper bound on the CP asymmetry in heavy neutrino decays which, together with the kinetic equations, yields an upper bound on all light neutrino masses of 0.1 eV. Lepton number changing processes at temperatures above the temperature T_B of baryogenesis can erase other, pre-existing contributions to the baryon asymmetry. We find that these washout processes become very efficient if the effective neutrino mass \tilde{m}_1 is larger than m_* \simeq 10^{-3} eV. All memory of the initial conditions is then erased. Hence, for neutrino masses in the range from (\Delta m^2_sol)^{1/2} \simeq 8*10^{-3} eV to (\Delta m^2_atm)^{1/2} \simeq 5*10^{-2} eV, which is suggested by neutrino oscillations, leptogenesis emerges as the unique source of the cosmological matter-antimatter asymmetry.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/03ded56ccc3f6b35c8675fbfa5b13081ae60e4c2

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Citations in the corpus

Running neutrino mass parameters in see-saw scenarios (2005, background): “The requirement of successful baryogenesis via thermal leptogenesis imposes constraints on fermion mass models and even places an upper bound on the mass of the light neutrinos [67].”
The Phenomenology of Right Handed Neutrinos (2013, background): “1 eV [392, 393]; see [394] for an review on the connection with neutrino masses.”
Leptogenesis (2008, unknown): “8) where mmin is the smallest light neutrino mass (this is relevant for degenerate light neutrino masses), and that “usually” m̃ >∼ msol [108] (see also [109]).”
A White Paper on keV sterile neutrino Dark Matter (2016, result): “1) eV [394, 398, 399, 436] an upper bound that now cosmological observations, in particular the new results from the Planck satellite, indicate to be respected.”
Type II leptogenesis and the neutrino mass scale (2004, background): “Together with an improved bound [13] on the type I decay asymmetry, this strongly increases the type I bound on MR1 [27] for increasing m ν min”
Leptogenesis in the Universe (2012, unknown): “t was found that successful leptogenesis with a hierarchical spectrum of the RH neutrinos 10 Neutrino Physics Leptogenesis in the Universe requires M 1 >˘109 GeV [61, 62, 63] and m 1 <˘0:1 eV [64, 65, 55, 66]. This bound implies that the RH neutrinos must be produced at temperatures T >˘10”
Running neutrino masses, mixings and CP phases: Analytical results and phenomenological consequences (2003, background): “In [42], an analytic expression for the maximal relevant CP asymmetry was derived,”