Abstract: Using the characteristical parameters of high speed solar wind observed by Ulysses,the energy flux distribution of high speed solar wind is obtained in the high latitudes.The results states clearly that the total energy flux density is about 2.1 × 10^-3J·m^-2·s^-1 (normalized to 1AU), mainly dominated by kinetic energy flux density (about 58%)and what overcome the gravitational potential energy flux at one solar radius (about 39%). In order to drive the high speed solar wind, the input energy flux density must be over 7.1×10²J·m^-2·s^-1 in the coronal source region of high speed solar wind.It is 40% larger than that of derivation from observations of previous satellites near the ecliptic plane. It is infered that there may exist two types of energy flux responsible for heating and accelerating the outflowing solar wind from the remote-sensing observations of the coronal source region. One has more short dissipatoon length, it will be dissipated within the very short space region (about 1-2R_s)and make the corona temperature rising up very quickly. The other is stored in the solar wind, it will be dissipated continuosly with the solar wind outflowing and accelerate the solar wind as well as heating solar wind.