Published April 1983
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Evolution of the ultra high energy cosmic ray spectrum by transport equation
Description
Ultra-high energy proton primaries interacting with the 30K photon background are treated as a transport phenomenon. Baryon number is explicitly conserved and the evolved spectrum develops a bump at a scale of order 5x1019 eV, below the cutoff, due to the pile-up of energy degraded protons. This may correspond in part to the observed ankle structure in the CR spectrum
Availability note (English)
MF available from INIS under the Report Number; Available from NTIS, PC A02/MF A01 as DE83013711.Files
14790035.pdf
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Additional details
Publishing Information
- Imprint Pagination
- 4 p.
- Report number
- FERMILAB-CONF--83/32-THY
Conference
- Title
- 18. international cosmic ray conference.
- Dates
- 22 Aug - 3 Sep 1983.
- Place
- Bangalore (India).
INIS
- Country of Publication
- United States
- Country of Input or Organization
- United States
- INIS RN
- 14790035
- Subject category
- S79: ASTROPHYSICS, COSMOLOGY AND ASTRONOMY;
- Resource subtype / Literary indicator
- Conference, Numerical Data
- Descriptors DEI
- BACKGROUND RADIATION; COSMIC PHOTONS; COSMIC PROTONS; COSMIC RAY PROPAGATION; ENERGY SPECTRA; EXPERIMENTAL DATA; PRIMARY COSMIC RADIATION
- Descriptors DEC
- BARYONS; CATIONS; CHARGED PARTICLES; COSMIC RADIATION; DATA; ELEMENTARY PARTICLES; FERMIONS; HADRONS; HYDROGEN IONS; HYDROGEN IONS 1 PLUS; INFORMATION; IONIZING RADIATIONS; IONS; MASSLESS PARTICLES; NUCLEONS; NUMERICAL DATA; PHOTONS; PROTONS; RADIATIONS; SPECTRA
Optional Information
- Secondary number(s)
- CONF-830830--4.