Abstract

An analysis of the data of spacecraft that scanned large areas of the heliosphere, as well as the results of magnetohydrodynamic calculations, indicates that corotating interaction regions of solar wind (SW), which are almost always present in the low- and mid-latitude heliosphere, sometimes strongly change the large-scale characteristics of the heliosphere that are important for long-term variations in the intensity of galactic cosmic rays (GCRs). In particular, for Carrington rotation no. 2066 (January–February 2008), these regions enhance magnetic fields in the inner (r < 3–5 AU) heliosphere and weaken them in the middle and far heliosphere, as well as significantly changing the polarity distribution of heliospheric magnetic fields. The assumption is made that in this situation the influence of the corotating interaction regions should lead to an increase in the GCR intensity in many regions of the heliosphere. This paper discusses the process of changing the polarity distribution of heliospheric magnetic fields due to the interaction of SW streams for Carrington rotation no. 2066 of different speeds, the simple model of the heliospheric magnetic field without an interaction between the SW streams of different speeds, as well as the results of numerical two-dimensional finite-difference calculations of longitude-averaged GCR intensity with the use of this model in comparison with a three-dimensional Monte Carlo calculation based on three-dimensional magnetohydrodynamic simulation of the heliosphere.

中文翻译：

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太阳风相互作用的同转区域对银河宇宙线强度长期变化的影响

摘要

对扫描大面积日光层的航天器数据以及磁流体动力学计算结果的分析表明，太阳风（SW）的共转相互作用区域几乎总是存在于中低纬度日光层中，有时会强烈改变日光层的大尺度特征，这对于银河宇宙射线（GCR）强度的长期变化很重要。特别是对于卡林顿轮换来说，没有。2066年（2008年1月至2月），这些区域增强了内日光层（r < 3-5 AU）的磁场，削弱了中远日光层的磁场，并显着改变了日光层磁场的极性分布。假设在这种情况下，共转相互作用区域的影响会导致日光层许多区域的 GCR 强度增加。本文讨论了卡林顿自转1号由于SW流的相互作用而改变日光层磁场极性分布的过程。不同速度的2066、不同速度的SW流之间没有相互作用的日光层磁场的简单模型，以及利用该模型对经度平均GCR强度进行数值二维有限差分计算的结果与基于日光层三维磁流体动力学模拟的三维蒙特卡罗计算进行比较。