An estimate of the secondary-proton spectrum at small atmospheric depths

SummaryWe have calculated the energy spectrum of secondary protons produced in the atmosphere as a function of the atmospheric depth and zenith angles at a location with zero geomagnetic cut-off. In this calculation, we have included all relevant energy losses and production processes. It is shown that the protons produced from the target nuclei through recoil and evaporation processes dominate the spectrum below 350 MeV. These calculations have been carried out over an energy region from 20 MeV to 40 GeV and up to a depth of 40 g/cm2 of the atmosphere over a latitude with zero geomagnetic cut-off for both the periods of minimum and maximum solar modulation.

[1]  G. R. Stevenson,et al.  Cosmic-Ray Hydrogen and Helium Nuclei during a Solar Quiet Time in July 1961 , 1964 .

[2]  A. Dar.  Particle production in cosmic ray collisions , 1979 .

[3]  J. Earl,et al.  Balloon measurements of cosmic ray protons and helium over half a solar cycle 1965–1969 , 1971 .

[4]  Bowen,et al.  Propagation and secondary production of low-energy antiprotons in the atmosphere. , 1986, Physical review. D, Particles and fields.

[5]  N. Digiacomo,et al.  MICROSCOPIC DESCRIPTION OF NUCLEON NUCLEUS TOTAL REACTION CROSS-SECTIONS , 1980 .

[6]  G. Smoot,et al.  A measurement of cosmic-ray rigidity spectra above 5 GV/c of elements from hydrogen to iron. , 1973 .

[7]  G. Smoot,et al.  Abundances and spectra for cosmic-ray nuclei from lithium to iron for 2 to 150 GeV per nucleon , 1978 .

[8]  J. Ormes,et al.  Proton and helium nuclei cosmic-ray spectra and modulations between 100 and 2000 Mev/nucleon , 1968 .

[9]  B. Teegarden.  A study of low-energy galactic cosmic rays from 1961 to 1965 , 1967 .

[10]  W. Webber,et al.  The charge composition and energy spectra of cosmic-ray nuclei from 3000 MeV per nucleon to 50 GeV per nucleon , 1978 .

[11]  J. Grunsfeld,et al.  Energy spectra and composition of primary cosmic rays , 1991 .

[12]  Webber,et al.  Total charge and mass changing cross sections of relativistic nuclei in hydrogen, helium, and carbon targets. , 1990, Physical review. C, Nuclear physics.

[13]  R. McGuire,et al.  The cosmic radiation in the heliosphere at successive solar minima , 1992 .

[14]  J. Arens,et al.  Energy spectra of cosmic-ray nuclei to above 100 GeV per nucleon , 1980 .

[15]  J. Simpson,et al.  The anomalous He-4 component in the cosmic-ray spectrum at below approximately 50 MeV per nucleon during 1972-1974 , 1975 .

[16]  J. Ormes,et al.  Measurement of cosmic-ray proton and helium spectra during the 1987 solar minimum , 1991 .

[17]  Peter Meyer,et al.  Charge Composition and Energy Spectra of Cosmic Ray Nuclei , 1974 .

[18]  P. Petkov,et al.  Evidence for strong ground-state shape asymmetry in even germanium and selenium isotopes , 1994 .

[19]  J. Simpson,et al.  Galactic deuterium and its energy spectrum above 20 Mev per nucleon. , 1966 .

[20]  J. Ormes,et al.  Cosmic ray proton and helium spectra above 50 GeV , 1971 .

[21]  D. Hofmann,et al.  The measurement at balloon heights of the low energy hydrogen and helium isotopes in the cosmic radiation at solar minimum, 1965 , 1967 .

[22]  C. Powell,et al.  The Study of Elementary Particles by the Photographic Method (C. MAYER-BRICKE) , 1960 .

[23]  P. Meyer,et al.  Charge composition and energy spectra of cosmic-ray nuclei at energies above 5 GeV per nucleon , 1977 .

[24]  J A Simpson,et al.  Elemental and Isotopic Composition of the Galactic Cosmic Rays , 1983 .

[25]  J. Simpson,et al.  Cosmic-Ray ^{2}H from Satellite Measurements, 1965-1969 , 1971 .

[26]  A. Morselli,et al.  Absolute spectrum and charge ratio of cosmic ray muons in the energy region from 0.2 GeV to 100 GeV at 600 m above sea level , 1993 .