根据行星际闪烁观测研究耀班一激波前后太阳风电子密度功率谱的变化

采用弱散射与薄屏近似模型，利用快速傅利叶变换和阿贝尔变换的方法，对１９７２年６月１５日耀斑一激波的行星际闪烁观测资料进行了计算，分别计算了激波前与激波后的电子密度功率谱．发现在小波数段都具有幂函数形式，并且波后幂指数值略大于波前幂指数值．说明此例激波过后小波数段功率谱略变陡。

STUDY OF VARIATION THE CHANGE IN THE ELECTRON DENSITY POWER SPECTRA OF SOLAR WIND BEFORE AND AFTER A FLARE-SHOCK USING OBSERVED Ips DATA

Applying the weak scattering and thin-screen approximation model,we have evaluated the observation data on the interplanetary scintillation(IPS)of a flareshock on June 15, 1972 by the use of the FFT and Abel transfer approaches.The electron density power spectra of solar wind before and after the shock are computed,respectively. The results suggest that the spectra are in the form of a power law function at small wave numbers (0.001 to 0.009km).The power law index after the shock are greater than those before the shock,implying that the power spectra at the small wave number range become slightly steeper after passing through the shock.