Abstract Given recent successes in modelling the transport of cosmic rays (CRs) in the heliosphere from first principles, taking into account the behaviour of heliospheric turbulence quantities and their influence on the transport parameters of these particles in a manner as self-consistent as possible, the question naturally arises as to what insights such a modelling approach can yield when applied to the historical study of cosmic ray transport. The temporal relationship between the heliospheric magnetic field (HMF) and observed CR intensities at Earth during solar cycle 20 has long been regarded as anomalous with respect to other solar cycles. The present study presents an analysis of historic HMF observations that gleans information as to the behaviour of turbulence quantities during this period. This information is used to analyse CR transport coefficients, which are incorporated into a stochastic CR modulation code. Galactic CR intensities so computed are compared with observations, and it is demonstrated that this approach yields a temporal intensity profile in qualitative agreement with that displayed by neutron monitor observations, thereby providing new insights as to CR modulation in solar cycle 20.

中文翻译：

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更深入地了解太阳周期 20 期间的历史宇宙射线调制

摘要 鉴于最近在从第一性原理模拟日光层中宇宙射线 (CR) 传输方面取得的成功，考虑到了日光层湍流量的行为及其对这些粒子传输参数的影响，以尽可能自洽的方式，当应用于宇宙射线传输的历史研究时，自然会产生这样的问题，即这种建模方法可以产生什么见解。在太阳活动周期 20 期间，太阳圈磁场 (HMF) 与在地球观测到的 CR 强度之间的时间关系长期以来一直被认为与其他太阳周期相比是反常的。本研究对历史 HMF 观测进行了分析，这些观测收集了有关此期间湍流量行为的信息。该信息用于分析 CR 传输系数，这些系数被合并到随机 CR 调制代码中。将如此计算的银河 CR 强度与观测进行比较，并且证明这种方法产生的时间强度剖面与中子监测观测显示的定性一致，从而为太阳周期 20 中的 CR 调制提供了新的见解。