Abstract
The precision measurements of the monthly cosmic ray fluxes with Alpha Magnetic Spectrometer on the International Space Station are presented. Individual electron, positron, proton and helium spectra have been measured for each Bartel’s rotation period (27 days) in the time range from May 2011 to May 2017. This period covers the ascending phase of solar cycle #24 together with the reversal of the Sun’s magnetic field polarity through the minimum. The fluxes reveal a characteristic time dependence below 20 GeV. The data show a strong charge-sign dependent effects corresponding to the the polarity reversal of the solar magnetic field.
Highlights
The study of Cosmic Rays (CR) constitutes a unique instrument for understanding our universe
The solar activity has a cycle of ∼11 years, during which it increases reaching a maximum and decreases again
A detailed study of the CR fluxes evolution with time is needed in order to develop and test different models of the Solar Modulation (SM) effects based on the interaction of cosmic rays with the Heliosphere
Summary
The study of Cosmic Rays (CR) constitutes a unique instrument for understanding our universe. CR spectra, when measured near Earth, are significantly affected by the solar activity. The intensity of cosmic ray radiation is anti-correlated with the activity of the sun [1], and this is the so called Solar Modulation (SM) effect. A detailed study of the CR fluxes evolution with time is needed in order to develop and test different models of the SM effects based on the interaction of cosmic rays with the Heliosphere. The simultaneous measurements of e− and e+ (or p and p) over a complete solar activity cycle can represent a sound test of the current charge-sign dependent modulation models. AMS-02 can provide the most accurate measurements of the time dependence of particle and anti-particle fluxes since 2011 thanks to its high acceptance and the excellent performance of the detector. The time variation of CR electron (e−), positron (e+), proton (p) and Helium (He) fluxes during the first 6 years of data taking will be presented
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