极性反转期间太阳调制模型的新情景
A New Scenario of Solar Modulation Model during the Polarity Reversing
AI总结：
本研究利用SOLARPROP和机器学习模拟银河宇宙射线传播，发现第24太阳活动周极大期间太阳调制参数峰值在2014年2月，考虑粒子传播时间后推迟至11月，存在九个月时间滞后。
摘要：
当银河宇宙射线（GCRs）进入日球层时，它们会遇到太阳风等离子体，其强度会降低，这被称为太阳调制。这种调制是由几个因素共同引起的，如粒子能量、太阳活动和太阳扰动。在本工作中，采用二维数值方法，利用SOLARPROP模拟GCRs在日球层中的传播，并为了克服耗时问题，还应用了机器学习技术。基于从旅行者1号和AMS-02观测得到的质子局域星际谱（LIS），我们找到了第24太阳活动周极大期间的太阳调制参数。结果表明，扩散系数的归一化和指数确实在2014年2月达到最大值。然而，在考虑了不同能量粒子的传播时间后，峰值时间被推迟到2014年11月，正如预期的那样。这九个月的延迟被称为时间滞后。
英文摘要：
When the Galactic Cosmic Rays (GCRs) entering the heliosphere, they encounter the solar wind plasma, and their intensity is reduced, so-called solar modulation. The modulation is caused by the combination of a few factors, such as particle energies, solar activity and solar disturbance. In this work, a 2D numerical method is adopted to simulate the propagation of GCRs in the heliosphere with SOLARPROP, and to overcome the time-consuming issue, the machine learning technique is also applied. With the obtained proton local interstellar spectra (LIS) based on the observation from Voyager 1 and AMS-02, the solar modulation parameters during the solar maximum activity of cycle 24 have been found. It shows the normalization and index of the diffusion coefficient indeed reach a maximal value in February 2014. However, after taking into account the travel time of particles with different energies, the peak time was found postponed to November 2014 as expected. The nine-month late is so-called time lag.
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