Gas dynamic models of solar flares

An electron flux with spectrum Esub(0)sup(-sigma)/Esub(0) (>=) 10 keV/100 sec is insident from corona into chromosphere. Temperature, velocity, density and ionization distribution is calculated with regard to gas viscosity when sigma = 3,4,5,6 and at every sigma for four values of particle energy flux F0=4x109, 1010,1011, 1012 egrsxch-2sec-1 at the stages of heating and cooling in open and closed models of the flash region. The main conclusions drawn earlier on the basis of a poorly estimated material, remain unchanged. It has become possible to obtain gas heating by a Shock wave and to consider the effect of an intense energy flux with regard to viscosity. The peculiarities of heating and cooling in a closed model, which conforms to the structure of the magnetic field of an arch type, whose ends are in photosphere are brought out. A great variety of values of the parameters, which characterize physical condition in the flash region, is obtained