The cosmic-ray proton and helium spectra measured with the CAPRICE98 balloon experiment

被引：112

作者：

Boezio, M

Bonvicini, V

Schiavon, P

Vacchi, A

Zampa, N

Bergström, D

Carlson, P

Francke, T

Hansen, P

Mocchiutti, E ^{[1
]}

Suffert, M

Hof, M

Kremer, J

Menn, W

Simon, M

Ambriola, M

Bellotti, R

Cafagna, F

Ciacio, F

Circella, M

De Marzo, CN

Finetti, N

Papini, P

Piccardi, S

Spillantini, P

Vannuccini, E

Bartalucci, S

Ricci, M

Casolino, M

De Pascale, MP

Morselli, A

Picozza, P

Sparvoli, R

Mitchell, JW

Ormes, JF

Stephens, SA

Streitmatter, RE

Bravar, U

Stochaj, SJ

机构：

[1] AlbaNova Univ Ctr, SCFAB, KTH, Royal Inst Technol, S-10691 Stockholm, Sweden

[2] Sezione INFN Trieste, I-34147 Trieste, Italy

[3] Univ Trieste, I-34147 Trieste, Italy

[4] New Mexico State Univ, RL Golden Particle Astrophys Lab, Las Cruces, NM 88003 USA

[5] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[6] Univ Roma Tor Vergata, I-00133 Rome, Italy

[7] Sezione INFM Roma 2, I-00133 Rome, Italy

[8] Ist Nazl Fis Nucl, Lab Nazl Frascati, I-00044 Frascati, Italy

[9] Univ Florence, I-50125 Florence, Italy

[10] Sezione INFN Firenze, I-50125 Florence, Italy

[11] Univ Bari, I-70126 Bari, Italy

[12] Sezione INFN Bari, I-70126 Bari, Italy

[13] Univ Siegen, D-57068 Siegen, Germany

[14] Ctr Rech Nucl, F-67037 Strasbourg, France

来源：

ASTROPARTICLE PHYSICS | 2003年 / 19卷 / 05期

基金：

美国国家航空航天局;

关键词：

cosmic rays; elementary particles; RICH detectors; balloons;

D O I：

10.1016/S0927-6505(02)00267-0

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

A new measurement of the primary cosmic-ray proton and helium fluxes from 3 to 350 GeV was carried out by the balloon-borne CAPRICE experiment in 1998. This experimental setup combines different detector techniques and has excellent particle discrimination capabilities allowing clear particle identification. Our experiment has the capability to determine accurately detector selection efficiencies and systematic errors associated with them. Furthermore, it can check for the first time the energy determined by the magnet spectrometer by using the Cherenkov angle measured by the RICH detector well above 20 GeV n(-1). The analysis of the primary proton and helium components is described here and the results are compared with other recent measurements using other magnet spectrometers. The observed energy spectra at the top of the atmosphere can be represented by (1.27 +/- 0.09) x 10(4) E-2.75+/-0.02 particles (m(2) GeV sr s)(-1), where E is the kinetic energy in GeV, for protons between 20 and 350 GeV and (4.8 +/- 0.8) X 10(2) E-2 67+/-0.03 particles (m(2) GeV n(-1) sr s)(-1), where E is the kinetic energy in GeV per nucleon, for helium nuclei between 15 and 150 GeV n(-1). (C) 2003 Elsevier Science B.V. All rights reserved.

引用

页码：583 / 604

页数：22

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BERGSTROM D, THESIS ROYAL I TECHN

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