Creation of photons and electron - positron pairs by a neutrino in a strong magnetic field

An influence of a strong external magnetic field on the neutrino self-energy operator is investigated. The width of the neutrino decay into the electron and W boson, and the mean free path of an ultra-high energy neutrino in a strong magnetic field are calculated. A kind of energy cutoff for neutrinos propagating in a strong field is defined.

The decay of magneto-plasma into neutrino anti-neutrino pair has been studied in the framework of the electro-weak interaction theory. The decay rate is calculated and the expression for the energy-loss rate is obtained in the extreme relativistic case. The neutrino luminosity has also been computed for a neutron star. A comparative study between the decay of magneto-plasma and the ordinary plasma neutrino process has been outlined in view of the cooling of highly magnetized ...

We calculate the neutrino luminosity of a degenerate electron gas in a strong magnetic field via plasmon decay to a neutrino pair due to neutrino electromagnetic moments and obtain the relative upper bounds on the effective neutrino magnetic moment.

The processes of neutrino (antineutrino) absorption and electron (positron) capture on nucleons provide the dominant mechanisms for heating and cooling the material between the protoneutron star and the stalled shock in a core-collapse supernova. Observations suggest that some neutron stars are born with magnetic fields of at least 10^15 G while theoretical considerations give an upper limit of 10^18 G for the protoneutron star magnetic fields. We calculate the rates for the ...

High energy neutrino bremsstrahlung $\nu \to \nu + \gamma$ in a strong magnetic field ($B \gg B_s$) is studied in the framework of the Standard Model (SM). A resonance probability and a four-vector of the neutrino energy and momentum loss are presented. A manifestation of the neutrino bremsstrahlung in astrophysical cataclysm of type of a supernova explosion or a merger of neutron stars, such as an possible origin of cosmological $\gamma$-burst is discussed.

The processes of electron neutrino capture on neutron and electron anti-neutrino capture on proton, and their reverse processes provide the dominant mechanisms for heating and cooling the material below the stalled shock in a core-collapse supernova. We summarize the major effects of strong magnetic fields on the rates of the above reactions and illustrate these effects with a simple supernova model. Due to parity violation of weak interaction the heating rates are asymmetric...

Production of a massive neutrino-antineutrino pair by a virtual polarized photon in the Weiberg-Salam model with mixing is studied. The rate of the neutrino production by photons with various polarizations is found at values of the magnetic field intensity lower than critical.

The process of pair creation by a photon in a strong magnetic field is investigated basing on the polarization operator in the field. The total probability of the process is found in a relatively simple form. The probability exhibits a "saw-tooth" pattern because of divergences arising when the electron and positron are created at threshold of the Landau energy levels. The pattern will be washed out at averaging over any smooth photon energy distribution. The new results are ...

We present the calculation of the probability production of an electron-positron pair in the presence of a strong magnetic field with time-varying strength. The calculation takes into account the presence of a strong, constant and uniform gravitational field in the same direction of the magnetic field. The results show that the presence of the gravitational field in general enhances the production of pairs. In particular, high-energy pairs are more likely produced in the pres...

The electron-positron pair production by an electron in a strong magnetic field near the process threshold is considered. The process is shown to be more probable if the spin of the initial electron is oriented along the field. In this case, the probability of the process is $\sim10^{13} s^{-1}$ when the magnetic field strength is $H=4\cdot 10^{12}$ G.