【摘要】 根据Ylysses观测，比较完整地计算了高纬行星际空间太阳风能流分布．计算表明，行星际空间的高速流能流密度约为2．1×10-3J·m-2·s-1（日心距离r＝1AU），主要来自于太阳风离子所携带的动能流（占58％）和克服太阳引力的势能流（占39％）．要驱动高速流，需要在日冕底部高速流源区（日心距离r=1Rs）向外输出到太阳风的能流密度为7．1×102J·m-2·s－1·分析表明，由日冕底部向外可能输出两种形式的能流，其中一种具有较短的耗散长度，被耗散在很短的空间区域（～1—2Rs），使日冕温度迅速提高。另一种储藏在连续向外传播的太阳风中，不断耗散用以加速太阳风（＞2Rs）．更多还原

【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 1-2Rs) 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.更多还原