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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 07692naa a2201921 4500 | |
| 001 | oai:DiVA.org:lnu-30289 | |
| 003 | SwePub | |
| 008 | 131108s2004 | |||||||||||000 ||eng| | |
| 024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-302892 URI |
| 024 | 7 | a https://doi.org/10.1016/j.astropartphys.2003.10.0042 DOI |
| 040 | a (SwePub)lnu | |
| 041 | a engb eng | |
| 042 | 9 SwePub | |
| 072 | 7 | a ref2 swepub-contenttype |
| 072 | 7 | a art2 swepub-publicationtype |
| 100 | 1 | a Aglietta, M4 aut |
| 245 | 1 0 | a The cosmic ray primary composition between 10(15) and 10(16) eV from Extensive Air Showers electromagnetic and TeV muon data |
| 264 | 1 | b Elsevier,c 2004 |
| 338 | a print2 rdacarrier | |
| 520 | a The cosmic ray primary composition in the energy range between 10(15) and 10(16) eV, i.e., around the "knee" of the primary spectrum, has been studied through the combined measurements of the EAS-TOP air shower array (2005 m a. s.l., 10(5) m(2) collecting area) and the MACRO underground detector (963 m.a.s.l., 3100 m w.e. of minimum rock overburden, 920 m(2) effective area) at the National Gran Sasso Laboratories. The used observables are the air shower size (N-c) measured by EAS-TOP and the muon number (N-mu) recorded by MACRO. The two detectors are separated on average by 1200 m of rock, and located at a respective zenith angle of about 30degrees. The energy threshold at the surface for muons reaching the MACRO depth is approximately 1.3 TeV. Such muons are produced in the early stages of the shower development and in a kinematic region quite different from the one relevant for the usual N-mu - N-e studies. The measurement leads to a primary composition becoming heavier at the knee of the primary spectrum, the knee itself resulting from the steepening of the spectrum of a primary light component (p, He) of Deltay = 0.7 +/- 0.4 at E-0 similar to 4 x 10(15) eV. The result confirms the ones reported from the observation of the low energy muons at the surface (typically in the GeV energy range), showing that the conclusions do not depend on the production region kinematics. Thus, the hadronic interaction model used (CORSIKA/QGSJET) provides consistent composition results from data related to secondaries produced in a rapidity region exceeding the central one. Such an evolution of the composition in the knee region supports the "standard" galactic acceleration/propagation models that imply rigidity dependent breaks of the different components.. and therefore breaks occurring at lower energies in the spectra of the light nuclei. (C) 2003 Elsevier B.V. All rights reserved. | |
| 650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
| 653 | a Astropartikelfysik | |
| 653 | a Astroparticle Physics | |
| 700 | 1 | a Alessandro, B4 aut |
| 700 | 1 | a Antonioli, P4 aut |
| 700 | 1 | a Arneodo, F4 aut |
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| 700 | 1 | a Bertaina, M4 aut |
| 700 | 1 | a Castagnoli, C4 aut |
| 700 | 1 | a Castellina, A4 aut |
| 700 | 1 | a Chiavassa, A4 aut |
| 700 | 1 | a Cini, G4 aut |
| 700 | 1 | a Piazzoli, B D4 aut |
| 700 | 1 | a Di Sicascio, G4 aut |
| 700 | 1 | a Fulgione, W4 aut |
| 700 | 1 | a Galeotti, P4 aut |
| 700 | 1 | a Ghia, P L4 aut |
| 700 | 1 | a Iacovacci, M4 aut |
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| 700 | 1 | a Morello, C4 aut |
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| 700 | 1 | a Valchierotti, S4 aut |
| 700 | 1 | a Vallania, P4 aut |
| 700 | 1 | a Vernetto, S4 aut |
| 700 | 1 | a Vigorito, C4 aut |
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| 700 | 1 | a Antolini, R4 aut |
| 700 | 1 | a Baldini, A4 aut |
| 700 | 1 | a Barbarino, G C4 aut |
| 700 | 1 | a Barish, B C4 aut |
| 700 | 1 | a Battistoni, G4 aut |
| 700 | 1 | a Becherini, Yvonneu Università di Bologna, Italy ; INFN, Italy4 aut0 (Swepub:lnu)yvbeaa |
| 700 | 1 | a Bellotti, R4 aut |
| 700 | 1 | a Bemporad, C4 aut |
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| 700 | 1 | a Bilokon, H4 aut |
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| 700 | 1 | a Carboni, M4 aut |
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| 700 | 1 | a Cecchini, S4 aut |
| 700 | 1 | a Cei, F4 aut |
| 700 | 1 | a Chiarella, V4 aut |
| 700 | 1 | a Choudhary, B C4 aut |
| 700 | 1 | a Coutu, S4 aut |
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| 700 | 1 | a Katsavounidis, E4 aut |
| 700 | 1 | a Katsavounidis, I4 aut |
| 700 | 1 | a Kearns, E4 aut |
| 700 | 1 | a Kim, H4 aut |
| 700 | 1 | a Kyriazopoulou, S4 aut |
| 700 | 1 | a Lamanna, E4 aut |
| 700 | 1 | a Lane, C4 aut |
| 700 | 1 | a Levin, D S4 aut |
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| 700 | 1 | a Mazziotta, M N4 aut |
| 700 | 1 | a Michael, D G4 aut |
| 700 | 1 | a Monacelli, P4 aut |
| 700 | 1 | a Montaruli, T4 aut |
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| 700 | 1 | a Peck, C W4 aut |
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| 700 | 1 | a Petrera, S4 aut |
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| 700 | 1 | a Walter, C W4 aut |
| 700 | 1 | a Webb, R4 aut |
| 710 | 2 | a Università di Bologna, Italy ; INFN, Italy4 org |
| 773 | 0 | t Astroparticle physicsd : Elsevierg 20:6, s. 641-652q 20:6<641-652x 0927-6505x 1873-2852 |
| 856 | 4 | u http://arxiv.org/pdf/astro-ph/0305325 |
| 856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-30289 |
| 856 | 4 8 | u https://doi.org/10.1016/j.astropartphys.2003.10.004 |
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