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Composition of primary cosmic rays at energies 10(15) to approximately 10(16) ev
| Content Provider | NASA Technical Reports Server (NTRS) |
|---|---|
| Author | Sato, K. Kobayashi, T. Mikumo, E. Yuda, T. Kasahara, K. Mito, I. Hotta, N. Amenomori, M. Konishi, E. Mizutani, K. |
| Copyright Year | 1985 |
| Description | The sigma epsilon gamma spectrum in 1 approx. 5 x 1000 TV observed at Mt. Fuji suggests that the flux of primary protons 10 to the 15 approx 10th eV is lower by a factor of 2 approx. 3 than a simple extrapolation from lower energies; the integral proton spectrum tends to be steeper than around to the power V and the spectral index tends to be steeper than Epsilon to the -17th power around 10 to the 14th power eV and the spectral index becomes approx. 2.0 around 10 to the 15th power eV. If the total flux of primary particles has no steepening up to approx 10 to the 15th power eV, than the fraction of primary protons to the total flux should be approx 20% in contrast to approx 45% at lower energies. |
| File Size | 266958 |
| Page Count | 4 |
| File Format | |
| Alternate Webpage(s) | http://archive.org/details/NASA_NTRS_Archive_19850025748 |
| Archival Resource Key | ark:/13960/t55f3px35 |
| Language | English |
| Publisher Date | 1985-08-01 |
| Access Restriction | Open |
| Subject Keyword | Space Radiation Protons Cosmic Ray Showers Flux Density Energy Spectra Particle Emission Energy Distribution Secondary Cosmic Rays Particle Density Concentration Electron Distribution Monte Carlo Method Ntrs Nasa Technical Reports Server (ntrs) Nasa Technical Reports Server Aerodynamics Aircraft Aerospace Engineering Aerospace Aeronautic Space Science |
| Content Type | Text |
| Resource Type | Article |
