The flux of cosmic ray hadrons at the atmospheric depth of 820 g cm(-2) has been measured by means of the EASTOP hadron calorimeter (Campo Imperatore, National Gran Sasso Laboratories, 2005 m a.s.l.). The hadron spectrum is well described by a single power law: S-h(E-h) = (2.25 +/- 0.21 +/- 0.34(sys)) x 10(-7) [GRAPHICS] m(-2)s(-1)sr(-1)GeV(-1) over the energy range 30 GeV-30 TeV. The procedure and the accuracy of the measurement are discussed. The primary proton spectrum is derived from the data by using the CORSIKA/QGSJET code to compute the local hadron flux as a function of the primary proton spectrum and to calculate and subtract the heavy nuclei contribution (basing on direct measurements). Over a wide energy range E-0 = 0.5-50 TeV its best fit is given by a single power law: S(E-0) = (9.81 +/- 1.1 +/- 1.6(sys)) x 10(-5) [GRAPHICS] m(-2)s(-1)sr(-1)GeV(-1).
Measurement of the cosmic ray hadron spectrum up to 30 TeV at mountain altitude: the primary proton spectrum / M., Aglietta; B., Alessandro; P., Antonioli; F., Arneodo; L., Bergamasco; M., Bertaina; C., Castagnoli; A., Castellina; A., Chiavassa; G. C., Castagnoli; D'ETTORRE PIAZZOLI, Benedetto; G. D., Sciascio; W., Fulgione; P., Galeotti; P. L., Ghia; Iacovacci, Michele; G., Mannocchi; C., Morello; G., Navarra; L., Riccati; O., Saavedra; G. C., Trinchero; S., Valchierotti; P., Vallania; S., Vernetto; C., Vigorito. - In: ASTROPARTICLE PHYSICS. - ISSN 0927-6505. - STAMPA. - 19:(2003), pp. 329-338. [10.1016/S0927-6505(03)00103-8]
Measurement of the cosmic ray hadron spectrum up to 30 TeV at mountain altitude: the primary proton spectrum
D'ETTORRE PIAZZOLI, BENEDETTO;IACOVACCI, MICHELE;
2003
Abstract
The flux of cosmic ray hadrons at the atmospheric depth of 820 g cm(-2) has been measured by means of the EASTOP hadron calorimeter (Campo Imperatore, National Gran Sasso Laboratories, 2005 m a.s.l.). The hadron spectrum is well described by a single power law: S-h(E-h) = (2.25 +/- 0.21 +/- 0.34(sys)) x 10(-7) [GRAPHICS] m(-2)s(-1)sr(-1)GeV(-1) over the energy range 30 GeV-30 TeV. The procedure and the accuracy of the measurement are discussed. The primary proton spectrum is derived from the data by using the CORSIKA/QGSJET code to compute the local hadron flux as a function of the primary proton spectrum and to calculate and subtract the heavy nuclei contribution (basing on direct measurements). Over a wide energy range E-0 = 0.5-50 TeV its best fit is given by a single power law: S(E-0) = (9.81 +/- 1.1 +/- 1.6(sys)) x 10(-5) [GRAPHICS] m(-2)s(-1)sr(-1)GeV(-1).I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
