Abstract

Solar wind is a set of flows with different parameters (the speed, the exponent of the spectrum of heterogeneities, the width, etc.). A bimodal character of the speed distribution of the solar wind was determined in spaceborne experiments. The measurements onboard the Ulysses spacecraft confirmed that the bimodal structure of solar wind continues to persist at relatively large distances from the Sun (to several astronomical units). However, there is one more possibility to determine the stream structure of solar wind. This is the method of interplanetary scintillations. The purpose of the paper is to reconstruct the stream structure of solar wind beyond the Earth’s orbit using the data on interplanetary scintillations obtained at two observational sites. The experiments were carried out at decameter wavelengths, since they are rather strongly scattered by the rarefied interplanetary plasma beyond the Earth’s orbit. The experimental data on interplanetary scintillations analyzed in this work were obtained in synchronous observations with the UTR-2 and URAN-2 radio telescopes. The parameters of solar wind and its stream structure were determined by comparison of the characteristics of interplanetary scintillations measured in the experiment (the dependences of the harmonic velocity of the cross-spectrum of scintillations and the power spectra) to those calculated with the models. To separate the interplanetary and ionospheric scintillations, the spectral, spatial, and frequency criteria were used. The results of this analysis show that solar wind beyond the Earth’s orbit consists of several streams that replace each other on the line of sight toward the radio source. These investigations prove the reliability and efficiency of the interplanetary scintillation method for reconstructing the stream structure of solar wind.

中文翻译：

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超出地球轨道的太阳风的大规模结构：使用分米无线电范围内两点星际闪烁测量数据重建

摘要

太阳风是一组具有不同参数（速度，异质性谱的指数，宽度等）的流。在航天实验中确定了太阳风速度分布的双峰特征。尤利西斯号上的尺寸航天器证实，太阳风的双峰结构在距太阳相对远的距离（到几个天文单位）上仍持续存在。但是，确定太阳风的流结构还有另一种可能性。这是行星际闪烁的方法。本文的目的是利用两个观测点获得的行星际闪烁数据重建太阳风在地球轨道以外的流结构。实验是在数十米的波长下进行的，因为它们被稀少的行星际等离子体强烈地散射到地球轨道以外。在这项工作中分析的关于行星际闪烁的实验数据是通过使用UTR-2和URAN-2射电望远镜进行同步观测获得的。通过比较实验中测量到的行星际闪烁的特征（闪烁的交叉谱的谐波速度和功率谱的依赖性）与通过模型计算得到的特征，来确定太阳风及其流结构的参数。为了分开行星际和电离层闪烁，使用了频谱，空间和频率标准。分析结果表明，超出地球轨道的太阳风由几束流组成，这些束流在朝向无线电源的视线中相互替代。这些研究证明了星际闪烁法重建太阳风流结构的可靠性和效率。