arXiv 1509.076522015-09-25astro-ph.SR

太阳风中的湍流密度起伏

Turbulent density fluctuations in the solar wind

Madhusudan Ingale

备注：: A PhD thesis

摘要：

由于太阳风中密度湍流引起的射电散射的处理通常采用相结构函数的渐近近似。我们使用一个一般的结构函数（GSF），跨越渐近极限和量化的相对误差的近似。我们表明，GSF预测准确的制度比它的渐近近似不仅是实际相关性，但内部尺度效应影响的散射加宽的估计。因此，我们建议GSF今后应用于散射展宽计算和估计的数量特征的密度湍流在日冕和太阳风。在这篇论文的下一部分，我们将利用先前发表的无线电波散射和行星际湍流观测资料，对太阳风中的密度湍流进行测量。密度波动推断使用GSF的无线电散射数据和现有的分析方法IPS。假设质子尺度下的密度波动是由于动力学Alfven波，我们限制的速度，在扩展的太阳风被加热，由于湍流耗散。这些结果提供了第一次估计的密度调制指数和太阳风加热率的所有方式从太阳到地球。

英文摘要：

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.

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