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Rays through the Earth’s geomagnetic field, and the forth step requires the use of particle/nuclear physicsįundamentals and atmosphere structure to transport the surviving incident cosmic rays through the Earth’sĪtmosphere to various depths. The third step requires geophysics to determine the trajectories of cosmic Solar wind magnetic field and the resulting interaction with the inward flow of galactic cosmic rays from the local The second requires knowledge of space physics to determine changing conditions in the Requires the application of astrophysics concepts to determine the spectrum and composition of cosmic rays at the Particle driftsĪre also considered in modulation theory to explain the observed charge sign dependent effects (Bieber et al., 1999 Ī complete calculation to determine particle fluxes in the atmosphere requires 4 major steps. Symmetric model of the heliosphere incorporating diffusion, adiabatic acceleration and convection. The modulated spectrum is generally determined by solving the Fokker-Planck equation for a spherical Solar modulation ofĬosmic ray fluxes has roughly a 22-year cycle, which must be considered to accurately predict the spectrum at anyĪdv. Wind that push charged particles out of the solar system or decelerate them (Fisk, 1971). Rays fluxes and the level of solar activity (solar modulation) is caused by magnetic field irregularities in the solar When solar activity is high, GCR flux is low and vice versa. The local flux of incident cosmic rays at a given time varies widely with geomagnetic location and the solar Vertically incident particles is appropriately called the vertical cutoff. Given location above the earth is called the geomagnetic cutoff rigidity for that point. The minimum momentum per unit charge (magnetic rigidity) an incident particle can have and still reach a Geomagnetic field provides a different kind of shielding, by deflecting low-momentum charged particles back into The atmosphere provides shielding, which at a givenĪltitude is determined by the mass thickness of the air above that altitude, called atmospheric depth. Vary with altitude, location in the geomagnetic field, and time in the sun’s magnetic activity cycle (Reitz, 1993 The intensity of the different particles making upĪtmospheric cosmic radiation, their energy distribution, and their potential effect on avionics and aircraft occupants Penetrate the magnetic fields of the solar system and the Earth, and reach the Earth’s atmosphere, they collide withĪtomic nuclei in air and create cascades of secondary radiation. Particles, though of different origin) with the remainder being heavier nuclei (Gaisser, 1990). The earth is continually bathed in high-energy ionizing radiation that comes from outside the solar system,Ĭalled galactic cosmic rays (GCR) which consist of roughly 90% protons and 9% helium nuclei (also called alp ha Results from this calculation are presented andĬompared to measurements. Points for each nucleon originating from a helium nucleus. This package interfaces with FLUKA to provide interaction starting Alpha particles are initially transported with a separate packageĬalled HEAVY to simulate fragmentation. Rigidity are transported through the atmosphere. For a given location, primaries above the effective cutoff
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Rigidity range of 0.5 GV - 20 TV uniform in CO&~. Primary protons and helium nuclei (alphas) are generated within the The propagation of primary particles through the Earth’s atmosphere is calculated with a three-dimensional MonteĬarlo transport program called FLUKA.
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Unique technique utilizing the Fokker-Plank equation with a non-linear rigidity-dependent diffusion coefficient, An improved global fit to the data was achieved through applying a On high altitude balloon flights and spacecraft. The primaryĬosmic ray spectrum has been modeled through an analysis of simultaneous proton and helium measurements made ’ Environmental Measurements Laboratory, US Department of Homeland Security, New York, NY 10014, USAĪ new computational procedure to determine particle fluxes in the Earth’s atmosphere is presented. ‘NASA Langley Research Center, Hampton, VA, 23681, USAģ Isti&o.Superiore di Sanita ‘, I-00161, Rome, Italy ’ Bartol Research Institute, University of Delaware, Newark, DE, 19716, USA Clem’, Giovanni De Angelis2.3, Paul Goldhagen4, John W. PROCEDURES FOR A NEW ATMOSPHERIC IONIZING