Majorana neutrino as Bogoliubov quasiparticle
نویسندگان
چکیده
منابع مشابه
Majorana neutrino mass
We treat 0+ → 2+ 0νββ decays taking into account recoil corrections to the nuclear currents. The decay probability can be written as a quadratic form of the effective coupling constants of the right-handed leptonic currents and the effective neutrino mass. We calculate the nuclear matrix elements for the 0+ → 21 0νββ decays of 76Ge and 100Mo, and demonstrate that the relative sensitivities of 0...
متن کاملRadiative Majorana Neutrino Masses
We present new radiative mechanisms for generating Majorana neutrino masses, within an extension of the standard model that successfully generates radiative charged lepton masses, order by order, from heavy sequential leptons. Only the new sequential neutral lepton has a right-handed partner, and its Majorana mass provides the seed for Majorana neutrino mass generation. Saturating the cosmolog-...
متن کاملMajorana Neutrino Mixing
The most plausible see-saw explanation of the smallness of the neutrino masses is based on the assumption that total lepton number is violated at a large scale and neutrinos with definite masses are Majorana particles. In this review we consider in details difference between Dirac and Majorana neutrino mixing and possibilities to reveal Majorana nature of neutrinos with definite masses.
متن کاملNeutrino: Dirac or Majorana?
The problem of the nature of the neutrino, namely if it is a massless Dirac particle different from its antineutrino or a Majorana particle with finite mass, is discussed. The question is related to the recent results showing the presence of neutrino oscillations clearly indicating that the difference between the squared mass of neutrinos of different flavours is different from zero. Neutrinole...
متن کاملElectron-Neutrino Majorana Mass and Solar Neutrino Oscillations
Assuming the Majorana masses of νe and the linear combination cντ − sνμ to be equal from their couplings to a heavy scalar triplet ξ, I show that their radiative splitting is given by ∆m2/m2ν = (3c /4π)(GF / √ 2)m2τ ln(m 2 ξ/m 2 W ). This is applicable to the small-angle matter-enhanced oscillation solution of the solar neutrino deficit and restricts mν to be between 0.20 and 0.36 eV if c 2 = 0...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Physics Letters B
سال: 2017
ISSN: 0370-2693
DOI: 10.1016/j.physletb.2017.09.051