The cosmic ray spectrum above 10(19) EV at Volcano Ranch and Haverah Park
The cosmic ray energy per particle spectrum above 10 to the 19th power eV is measured the same way that energy spectra are measured at much lower energies, by counting all of the particles in a specified energy range that are incident per unit time with trajectories within specified geometrical limi...
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ftnasantrs:oai:casi.ntrs.nasa.gov:19860022038 2023-05-15T18:45:26+02:00 The cosmic ray spectrum above 10(19) EV at Volcano Ranch and Haverah Park Linsley, J. Unclassified, Unlimited, Publicly available Feb 1, 1986 application/pdf http://hdl.handle.net/2060/19860022038 unknown Document ID: 19860022038 Accession ID: 86N31510 http://hdl.handle.net/2060/19860022038 No Copyright CASI SPACE RADIATION NASA. Goddard Space Flight Center Nineteenth International Cosmic Ray Conference. Conference Papers: Invited Rapporteur, Highlight, Miscellaneous, Volume 9; 12 p 1986 ftnasantrs 2016-06-11T22:51:59Z The cosmic ray energy per particle spectrum above 10 to the 19th power eV is measured the same way that energy spectra are measured at much lower energies, by counting all of the particles in a specified energy range that are incident per unit time with trajectories within specified geometrical limits. Difficulties with background or poorly known detection efficiency are markedly less than in some other cosmic ray measurements. The fraction of primary energy given to muons, neutrinos, and slow hadrons is less than 10% in this region, so the primary energy equals the track length integral of the secondary electrons with only a small correction for the energy given to other kinds of particles. Results from Volcano Ranch and Haverah Park are compared with results from the Yakutsk experiment. Other/Unknown Material Yakutsk NASA Technical Reports Server (NTRS) Yakutsk |
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SPACE RADIATION |
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SPACE RADIATION Linsley, J. The cosmic ray spectrum above 10(19) EV at Volcano Ranch and Haverah Park |
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SPACE RADIATION |
description |
The cosmic ray energy per particle spectrum above 10 to the 19th power eV is measured the same way that energy spectra are measured at much lower energies, by counting all of the particles in a specified energy range that are incident per unit time with trajectories within specified geometrical limits. Difficulties with background or poorly known detection efficiency are markedly less than in some other cosmic ray measurements. The fraction of primary energy given to muons, neutrinos, and slow hadrons is less than 10% in this region, so the primary energy equals the track length integral of the secondary electrons with only a small correction for the energy given to other kinds of particles. Results from Volcano Ranch and Haverah Park are compared with results from the Yakutsk experiment. |
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Other/Unknown Material |
author |
Linsley, J. |
author_facet |
Linsley, J. |
author_sort |
Linsley, J. |
title |
The cosmic ray spectrum above 10(19) EV at Volcano Ranch and Haverah Park |
title_short |
The cosmic ray spectrum above 10(19) EV at Volcano Ranch and Haverah Park |
title_full |
The cosmic ray spectrum above 10(19) EV at Volcano Ranch and Haverah Park |
title_fullStr |
The cosmic ray spectrum above 10(19) EV at Volcano Ranch and Haverah Park |
title_full_unstemmed |
The cosmic ray spectrum above 10(19) EV at Volcano Ranch and Haverah Park |
title_sort |
cosmic ray spectrum above 10(19) ev at volcano ranch and haverah park |
publishDate |
1986 |
url |
http://hdl.handle.net/2060/19860022038 |
op_coverage |
Unclassified, Unlimited, Publicly available |
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Yakutsk |
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Yakutsk |
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Yakutsk |
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Yakutsk |
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CASI |
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Document ID: 19860022038 Accession ID: 86N31510 http://hdl.handle.net/2060/19860022038 |
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No Copyright |
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1766236498858868736 |