标题： 太阳圈调制宇宙射线的时间和电荷符号依赖性 显示英文标题

标题： Time and Charge-Sign Dependence of the Heliospheric Modulation of Cosmic Rays

摘要： 同时且连续观测银河系宇宙射线电子和正电子的PAMELA和AMS02空间实验，最适合用于低于50 GeV的这些粒子在日球层调制的数值建模研究。 一个已建立的全面三维调制模型被用来计算电子和正电子的完整能谱，目的是重现覆盖前一个长期且不寻常的深太阳活动极小期以及最近包括太阳磁场极性反转在内的最大活动期的观测到的正电子/电子比值。 为此，首先建立了这些粒子的非常局部星际能谱。 我们的研究重点是主要调制过程，包括粒子漂移，以及其他参数如三个主要扩散系数是如何演变的，以及随后相应的电荷符号依赖的调制是如何发生的。 我们努力的最终结果是从2006年到2015年的正电子/电子的详细再现，显示了与主要观测特征的定性和定量一致。 特别是，我们确定了需要多少粒子漂移来解释每个太阳活动期间观测到的正电子/电子的时间依赖性，尤其是在没有明确磁极性的极性反转期间。 显示英文摘要

摘要： Simultaneous and continuous observations of galactic cosmic-ray electrons and positrons from the PAMELA and AMS02 space experiments are most suitable for numerical modeling studies of the heliospheric modulation of these particles below 50 GeV. A well-established comprehensive three-dimensional modulation model is applied to compute full spectra for electrons and positrons with the purpose of reproducing the observed ratio positrons/electrons for a period which covers the previous long and unusual deep solar minimum activity and the recent maximum activity phase including the polarity reversal of the solar magnetic field. For this purpose the very local interstellar spectra for these particles were established first. Our study is focused on how the main modulation processes, including particle drifts, and other parameters such as the three major diffusion coefficients, had evolved, and how the corresponding charge-sign dependent modulation had occurred subsequently. The end result of our effort is the detailed reproduction of positron/electrons from 2006 to 2015, displaying both qualitative and quantitative agreement with the main observed features. Particularly, we determine how much particle drifts is needed to explain the time dependence exhibited by the observed positron/electron during each solar activity phase, especially during the polarity reversal phase when no well-defined magnetic polarity was found.