A new method of calculating models for stellar coronae is being developed with the aim of providing models of coronae around hot stars capable of explaining the observed mass loss as a stellar wind from a hot corona. The method gives a stationary solution to the coupled equations of motion, continuity and energy balance. The equation of motion contains only the gradient of the gas pressure and the acceleration due to gravity. Radiation pressure is not yet included. The continuity equation assumes spherical symmetry. The energy equation includes heating by weak shock waves, heating by the absorption of photospheric radiation through continuous opacity, radiation losses, heating or cooling by conductivity and the effect on the energy balance of the velocity of the expanding atmosphere. The model is assumed to be optically thin. The velocity distribution is calculated from the solution going through the critical point.