标题： 太阳风中的湍流密度涨落 显示英文标题

标题： Turbulent density fluctuations in the solar wind

摘要： 太阳风中由于密度湍流引起的射电散射处理通常采用相位结构函数的渐近近似。 我们使用一种跨越渐近极限的一般结构函数（GSF），量化由这些近似引入的相对误差。 我们表明，GSF预测比其渐近近似的预测更准确的区域不仅具有实际意义，而且是在内尺度效应影响散射展宽估计的区域。 因此，我们建议今后应使用GSF进行散射展宽计算以及表征日冕和太阳风中密度湍流量的估算。 在本论文的下一部分，我们将利用之前发表的无线电波散射和行星际闪烁观测数据中的太阳风密度湍流测量值。 通过射电散射数据的GSF和现有IPS分析方法推断密度涨落。 假设质子尺度以下的密度涨落是由动能阿尔芬波引起的，我们限制了由于湍流耗散导致的扩展太阳风加热速率。 这些结果提供了从太阳到地球整个过程中密度调制指数和太阳风加热率的第一批估算值。 显示英文摘要

摘要： Treatments of the radio scattering due to density turbulence in the solar wind typically employ asymptotic approximations to the phase structure function. We use a general structure function (GSF) that straddles the asymptotic limits and quantify the relative error introduced by the approximations. We show that the regimes where GSF predictions are accurate than those of its asymptotic approximations is not only of practical relevance, but are where inner scale effects influence the estimate of the scatter-broadening. Thus we propose that GSF should henceforth be used for scatter broadening calculations and estimates of quantities characterizing density turbulence in the solar corona and solar wind. In the next part of this thesis we use measurements of density turbulence in the solar wind from previously publish observations of radio wave scattering and interplanetary scintillations. Density fluctuations are inferred using the GSF for radio scattering data and existing analysis methods for IPS. Assuming that the density fluctuations below proton scales are due to kinetic Alfv`en waves, we constrain the rate at which the extended solar wind is heated due to turbulent dissipation. These results provide the first estimates of the density modulation index and the solar wind heating rate all the way from the Sun to the Earth.