2005/05/31 by А. В. Кузнецов, A. V. Kuznetsov, Н. В. Михеев +4 · 4 citations
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Condensed matter physics #Dispersion relation #Electron #Field (mathematics) #Lepton #Magnetic field #Neutrino #Neutrino Physics Research #Nuclear physics #Particle physics #Particle physics theoretical and experimental studies #Physics #Quantum mechanics #hep-ph
paper · pdf · doi:10.1103/physrevd.73.023001
published as Phys.Rev.D73:023001,2006; Erratum-ibid.D73:029903,2006 · 9 pages, 1 figure, revtex. Version to appear in Phys. Rev. D (presentation improved, reference list revised, numerical error in Eq.(41) corrected, conclusions unchanged)
arxiv created 2005/12/13 · openalex publication_date 2006/01/05 · arxiv updated 2014/11/17 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We calculate the neutrino self-energy operator \ensuremathΣ(p) in the presence of a magnetic field B. In particular, we consider the weak-field limit eB\ensuremath≪m_\ensuremathℓ2, where m_\ensuremathℓ is the charged-lepton mass corresponding to the neutrino flavor \ensuremathν_\ensuremathℓ, and we consider a ``moderate field'' m_\ensuremathℓ2\ensuremath≪eB\ensuremath≪mW2. Our results differ substantially from the previous literature. For a moderate field, we show that it is crucial to include the contributions from all Landau levels of the intermediate charged lepton, not just the ground state. For the conditions of the early universe where the background medium consists of a charge-symmetric plasma, the pure B-field contribution to the neutrino dispersion relation is proportional to (eB)2 and thus comparable to the contribution of the magnetized plasma.