Beshley V. Non-thermal emission of adiabatic supernova remnants.

The thesis is devoted to the magnetohydrodynamic simulation of adiabatic evolution of supernova remnants, relativistic charged particles and non-thermal emission in supernova remnants in the classical theory of particle acceleration. The numerical and approximate analytical methods of calculations of spectra and building images of supernova remnants with taking into account the energy losses of particles (both electrons and protons) after leaving the field acceleration are developed in the work. The morphology of supernova remnants depends on the properties of the process of acceleration and orientation of the magnetic field are shown. Analyzing the images, resulting from the emission of electrons, tests for imposing restrictions on the properties of relativistic electrons populations and magnetic field have developed. In particular, a similar approach for protons showed that achieve two limbs structure surface brightness distribution of supernova remnants is possible only if the maximum energy of protons or the injection is not isotropic. The radial profiles of surface brightness supernova remnants in gamma-rays due to proton radiation can be used to estimate the concentration of molecular clouds that interacting with the supernova remnants are shown. The methods used for imposing constraints on the properties of supernova remnants 1006 and accelerated cosmic rays in it. It is shown that the average magnetic field in supernova remnants 1006 is a 32 microgauss and field intensity in the bright limb is 95 microgauss.