Galactic Cosmic Rays Production at the Equator and Magnetic Poles at the Minimum and Maximum Solar Activity

Abstract

Cosmic rays is composed of charged particles, created and possibly accelerated in the remains of supernovas. The measurement of cosmic ray fluxes allows to put constraints on their sources and their transport, but also to consider the problem of these radiations in the terrestrial environment. It is to answer these questions, that a numerical simulation code is established through the equations of HEAPS (1978) to evaluate this galactic flux in the upper atmosphere. The work proposed in this article is to estimate the production of galactic radiation at the equator and magnetic poles at the minimum and maximum of solar activity. On the other hand, the Sun emits a plasma which interacts with the particles of the cosmic radiation, modifying the fluxes resulting from the propagation in the galaxy. This modification evolves in time following the solar activity cycle and is called solar modulation. From this work, it appears that the magnetospheric geoefficiency depends on the geomagnetic latitude, and a high production at the magnetic poles. Since the cosmic ray intensity is affected by the interplanetary magnetic field, the galactic production is small during maximum solar activity and large at minimum solar activity.