Solar wind expansion with a heat-loss function

The problem of steady expansion of the solar wind is investigated allowing for heating and cooling mechanism in the medium. Single fluid equations are employed, neglecting viscosity and magnetic fields. It is found that the flow characteristics are modified in the regions near the Sun though the location of the critical point and the flow speeds beyond it are unaffected. It is surmised that the solar wind must originate at higher levels if it is subject to a heat-loss due to bremsstrahlung.