Abstract
Following recent observations which indicate the possibility of extremely high flow speeds in the inner corona, 700–800 km s−1 below 10 RS, and the possibility of very high proton temperatures, Tp⩽8.5×106 K, we present a new approach to solar wind modeling. In this approach we show that if the high proton temperatures in the inner corona are genuine, then flow speeds of 700 to 800 km s−1 can readily be achieved at 10 RS or even closer to the coronal base.
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