Modelling of sgr giant flares
Within the framework of the magnetar model SGR giant flares are investigated. The total X-ray flux of a relativistic plasma is calculated with taking into account a neutrino cooling, a decrease of X-ray emission area and a flux modulation by the neutron star rotation. The flux obtained is compared with data observed from the SGR 1900+14 giant flare. It is shown that a minimal value of the magnetar magnetic field strength is exist. Parameters of the X-ray emission area are estimated. The analysis shows that the predicted flux pulsating tail contradicts the existing observational data.