Input data that was used for this simulation.
Version: T96Year: 2014
DOY: 1
Hour: 0
Latitude: 45
Longitude: 90
Radius: 1
Rigidity step: 0.01 GV
Number of directions simulated: 1
Optimization level: Basic optimization
Spectrum: AMS-01
DST: -13 PDYN: 0.70 BY: 0.00 BZ: -4.10
Full asymptotic cone where intensity of incoming particles from different asymptotic direction is indicated by colors representing a part of the total registered intensity in percents. As spectrum at 1AU was used AMS-01 spectrum from region 10 (most poleward region, where influence of magnetosphere to cosmic rays was smallest).
Transmission function, denoted by black line, shows probability of particles from all directions with rigidity R to reach selected point inside magnetosphere.
Differential flux at the top of the atmosphere from vertically incoming trajectories (denoted by green color) and from multidirectional simulation(denoted by orange color). Spectrum ať the magnetopause is denoted by blue color.
Input data that was used for this simulation.
Version: T96Year: 2014
DOY: 1
Hour: 0
Latitude: 45
Longitude: 90
Radius: 1
Rigidity step: 0.01 GV
Number of directions simulated: 1
Optimization level: Basic optimization
Spectrum: AMS-01
DST: -13 PDYN: 0.70 BY: 0.00 BZ: -4.10
Spectra of allowed rigidities in selected directions.
Full asymptotic cone where intensity of incoming particles from different asymptotic direction is indicated by colors representing a part of the total registered intensity in percents. As spectrum at 1AU was used AMS-01 spectrum from region 10 (most poleward region, where influence of magnetosphere to cosmic rays was smallest).
Transmission function, denoted by black line, shows probability of particles from all directions with rigidity R to reach selected point inside magnetosphere.
Differential flux at the top of the atmosphere from vertically incoming trajectories (denoted by green color) and from multidirectional simulation(denoted by orange color). Spectrum ať the magnetopause is denoted by blue color.
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