In this paper a viscous, thermal conductive model of the solar wind is studied by using the NavierStokes equations to describe the motion of the solar wind. The fluid equations are reduced to a system of three first-order non-linear differential equations. The system of equations for this viscous model does not have a singular point at Mach T8 The asymptotic solution for this model shows that the temperature decreases according to , which is much faster than the results obtained for the inviscid model and the static model. The exact solution for this viscous model is obtained. For all values of the heliocentric distance r, its physical implication is discussed and compared with the observed data.
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Whang et al. (1966) studied this question.