Narrow Results

In this paper the formulae of magnetic susceptibility (MS) of charged particles are deduced in nonrelativistic and relativistic mean-field approximations in bulk matter. The analytic relativistic expression at high densities and strong fields, deduced for the de Hass–van Alphen (HVA) oscillation, shows that the oscillation frequency is proportional to the square of chemical potential and the reciprocal of the field, and is independent of the temperature. Numerical calculations are performed at finite temperatures and in a field range where the equation of state is not sensitive to the field. The nonoscillatory MS of the protoneutron star, which is dominated by the contributions of electrons (and light quarks, if deconfined) and is almost independent of the field, decreases as the protoneutron matter becomes denser. The numerical results for the HVA oscillation are also given. The oscillation amplitude becomes larger as the star becomes colder. We find that superposition of the HVA oscillations changes the oscillation properties drastically if the color deconfinement occurs at high densities.

Qualitative analysis of additional energy of neutrino and antineutrino in plasma is performed. A general expression for the neutrino self-energy operator is obtained in the case of ultra-high energies when the local limit of the weak interaction is not valid. The neutrino and antineutrino additional energy in plasma is calculated using the dependence of the W- and Z-boson propagators on the momentum transferred. The kinematical region for the neutrino radiative transition (the so-called "neutrino spin light") is established for some important astrophysical cases. For high energy neutrino and antineutrino, dominating transition channels in plasma, ν_e + e⁺ → W⁺, and , are indicated.

We review the recent progress in understanding the nature of gamma-ray bursts (GRBs). The occurrence of GRB is explained by the Induced Gravitational Collapse (IGC) in FeCO Core–Neutron star binaries and Neutron star–Neutron star binary mergers, both processes occur within binary system progenitors. Making use of this most unexpected new paradigm, with the fundamental implications by the neutron star (NS) critical mass, we find that different initial configurations of binary systems lead to different GRB families with specific new physical predictions confirmed by observations.