高频Alfven波供能的日冕及太阳风模型

A MODEL FOR THE SOLAR WIND AND CORONA WITH ENMRGY SUPPLIED BY HIGH FREQUENCY ALFVEN WAVES

空间探测的最新结果表明，太阳大气中广泛存在小尺度喷发事件，这些事件被认为是由新浮现磁通量导致的小尺度磁重联的表现．小尺度磁重联同时会产生高频Alfven波．本文给出了建立在上述思想基础上的描述日冕加热及太阳风加速的时变二元流体模型的一组数值解，显示解的时间演化、收敛特性及守恒特性．在对由过渡区发出的高频Alfven波频谱的适当假设下，数值解能够解释日冕及太阳风等多方面的观测结果，包括日冕加热，极冕洞密度径向变化，太阳风近日冕底部加速，及在03AU观测到的高速流特征．

A set of converging soluhons of a time dependent two-fluid model of the solarwind and the corona is presented. This model is based on the heating and accelerationeffects of high-frequency waves in the frequency range between lth and 400Hz. Thishigh frequency waves are assumed to be generated by the small-scale magnehc activityin the chromospheric network. The converging property of the solution and theconservation of the mass, momentUm and energy fluxes are also described. The modelresults can explain major properies observed in top transition region, corona and thehigh speed streams in the solar wind.