Abstract
A thorough understanding of solar effects on the galactic cosmic rays is relevant both to infer the local interstellar spectrum characteristics and to investigate the dynamics of charged particles in the heliosphere. We present a newly developed numerical modulation model to study the transport of galactic protons in the heliosphere. The model was applied to the 27-day averaged galactic proton flux recently released by the PAMELA and AMS02 experiments, covering an extended time period from mid-2006 to mid-2017.
Highlights
Most direct observations of Cosmic Rays (CRs) are made inside the heliosphere
The CR spectrum observed at Earth can differ significantly from the Local Interstellar Spectrum (LIS) due to many physical processes that modify the spectrum
This is true for CRs with kinetic energies below ∼20 GeV, which can be efficiently diffused, curved and de-accelerated adiabatically during their propagation from heliosphere to the Earth
Summary
The CR spectrum observed at Earth can differ significantly from the Local Interstellar Spectrum (LIS) due to many physical processes that modify the spectrum This is true for CRs with kinetic energies below ∼20 GeV, which can be efficiently diffused, curved and de-accelerated adiabatically during their propagation from heliosphere to the Earth. A thorough understanding of solar effects on the GCR propagation is relevant both to infer the LIS and to investigate the dynamics of charged particles in the heliosphere. It is important for astronauts and the electronic components radiation hazard during long-duration missions. The new precise data from AMS02 [1] and PAMELA [2] experiments offer a unique possibility to study the solar modulation over a long period of time
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