Kinetic models of solar and polar winds

The study of the solar corona has been strewn with great discoveries, surpr ises and controversies. The major steps since van de Hulst's (1953) and Cha pman's (1957) early hydrostatic models of the extended corona, until the mo st recent generations of kinetic models of the coronal expansion and of the supersonic solar wind flows, are presented. These models are compared to i n-situ observations. Progress in polar wind models went through a somewhat similar evolution that is outlined also. The advantages and limitations of the successive brands of solar wind and polar wind models are considered.