Radiation from collapsing stars

The particle dynamics and their non-thermal emission in the magnetospheres of collapsing stars are considered. When the stellar magnetosphere compresses under the collapse, its magnetic field increases considerably. Charged particles will be accelerated in this field. These particles will generate radiation when moving in the magnetic field. The collapsing stars can be a powerful sources of non-thermal radiation produced by the interaction of the charged particles with the magnetic field (Kryvdyk, 1999). The effect can be observed by modern instruments. The radiation flux grows during stellar collapse by a factor of millions and can be observed in the form of radiation pulse with duration equal to the stellar collapse time. The flux depends on the distance to the star, its magnetic field, and the particle spectrum in the magnetosphere. In this paper the radiation fluxes are calculated for various collapsing stars with initial dipole magnetic fields and initial power-law, relativistic Maxwell, and Boltzmann particle energy distributions in the magnetosphere.