Elementary Particle Interactions in Bkgd Magnetic Field by K. Bhattacharya

By K. Bhattacharya

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3 where Fig. 3a shows the contribution from the W exchange diagram and Fig. 3b shows the contribution from Z exchange. 15) where cV was defined in Eq. 44), m is the electronic mass, and Nµν = ∂µ (ψ (ν) γν Lψ(ν) ) − ∂ν (ψ (ν) γµ Lψ(ν) ) . 16) For energies much smaller than the electron mass, this can be used as an effective Lagrangian to calculate various processes involving photons and neutrinos in the presence of a background magnetic field Fµν . 17) where now fµν is the dynamical photon field, and look for the terms involving Fµν .

3. 4 describes the methods for handling ultraviolet divergences in calculations involving background magnetic fields. This chapter concludes with a general discussion on the various ideas exposed in the following sections. 2 Neutrino-photon scattering and the electromagnetic vertex of neutrinos In this section we will discuss effective neutrino photon interactions in a magnetized medium [32, 31], and the constituents of the neutrino photon electromagnetic vertex. But before taking up the issue of the ννγ vertex some comments on the neutrino-photon scattering in a background magnetic field follows.

It should be noted that the type of corrections to the dispersion relation discussed in Sec. 4 appear from chiral neutrinos. Thus, they produce chirality-preserving modifications to neutrino oscillations. In addition, if the neutrino has a magnetic moment, there will be chirality-flipping modifications as well. 5 As pointed out in chapter 1, they are not important for solar neutrinos, although may be important in other stellar objects like the neutron star where the magnetic fields are much larger.

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