C

A.A.G. bijdragen Pub Date : 1983-12-31 DOI:10.1515/9783112531327-005

I. Richterová, Z. Němeček, M. Beránek, J. Šafránková, J. Pavlů

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引用次数: 0

摘要

太阳风中相对氦丰度的突然变化通常归因于日冕中不同来源的太阳风流的边界。本文对氦丰度的快速变化进行了系统的研究，该研究支持这样一种观点，即大多数在短时间尺度(3-30秒)上的这些变化是由传输中的湍流产生的，这种湍流可能是由离子种类之间的速度差异驱动的。这种湍流有助于太阳风加热，并导致温度与氦丰度的相关性。关键词:太阳风在线资料:彩色图

本文章由计算机程序翻译，如有差异，请以英文原文为准。

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Abrupt changes of the relative He abundance in the solar wind are usually attributed to encounters with boundaries dividing solar wind streams from different sources in the solar corona. This paper presents a systematic study of fast variations of the He abundance that supports the idea that a majority of these variations on short timescales (3–30 s) are generated by in-transit turbulence that is probably driven by the speed difference between the ion species. This turbulence contributes to the solar wind heating and leads to a correlation of the temperature with He abundance. Key word: solar wind Online-only material: color figures

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A.A.G. bijdragen

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