EUV and radio observation, supplemented by other data, have made it possible to determine the flux of energy, F sub c, conducted from the corona into the chromosphere. Of the mechanical flux input in the corona, F sub m (of which F sub c is a large fraction), there are no direct measurements but limits can be found to it. It is shown that, if the described quantities relative to quiet regions are compared with the same quantities as observed in regions of different activity, it is possible to obtain important information on the regions of origin of the solar wind. In particular, it is found that the regions of very low EUV emission, i.e., the so-called coronal holes, appear to be the source of high energy streams of solar wind.