RELATIVE COMPOSITION AND ENERGY SPECTRA OF LIGHT NUCLEI IN COSMIC RAYS: RESULTS FROM AMS-01

被引：48

作者：

Aguilar, M. ^{[1
]}

Alcaraz, J. ^{[1
]}

Allaby, J. ^{[2
]}

Alpat, B. ^{[3
]}

Ambrosi, G. ^{[3
]}

Anderhub, H. ^{[4
]}

Ao, L. ^{[5
]}

Arefiev, A. ^{[6
]}

Arruda, L. ^{[9
]}

Azzarello, P. ^{[3
]}

Basile, M. ^{[7
,8
]}

Barao, F. ^{[9
,10
]}

Barreira, G. ^{[9
]}

Bartoloni, A. ^{[11
]}

Battiston, R. ^{[3
,12
]}

Becker, R. ^{[13
]}

Becker, U. ^{[13
]}

Bellagamba, L. ^{[7
,8
]}

Bene, P. ^{[14
]}

Berdugo, J. ^{[1
]}

Berges, P. ^{[13
]}

Bertucci, B. ^{[3
,12
]}

Biland, A. ^{[4
]}

Bindi, V. ^{[7
,8
]}

Boella, G. ^{[15
]}

Boschini, M. ^{[15
]}

Bourquin, M. ^{[14
]}

Bruni, G. ^{[7
,8
]}

Buenerd, M. ^{[16
]}

Burger, J. D. ^{[13
]}

Burger, W. J. ^{[12
]}

Cai, X. D. ^{[13
]}

Cannarsa, P. ^{[4
]}

Capell, M. ^{[13
]}

Casadei, D. ^{[7
,8
]}

Casaus, J. ^{[1
]}

Castellini, G. ^{[7
,8
,17
]}

Cernuda, I. ^{[1
]}

Chang, Y. H. ^{[18
]}

Chen, H. F. ^{[19
]}

Chen, H. S. ^{[20
]}

Chen, Z. G. ^{[5
]}

Chernoplekov, N. A. ^{[21
]}

Chiueh, T. H. ^{[18
]}

Choi, Y. Y. ^{[22
]}

Cindolo, F. ^{[7
,8
]}

Commichau, V. ^{[23
]}

Contin, A. ^{[7
,8
]}

Cortina-Gil, E. ^{[14
]}

Crespo, D. ^{[1
]}

机构：

[1] CIEMAT, Ctr Invest Energet Medioambientales & Tecnol, E-28040 Madrid, Spain

[2] CERN, European Lab Particle Phys, CH-1211 Geneva 23, Switzerland

[3] Ist Nazl Fis Nucl, Sez Perugia, I-06100 Perugia, Italy

[4] ETH, CH-8093 Zurich, Switzerland

[5] Chinese Acad Launching Vehicle Technol, CALT, Beijing 100076, Peoples R China

[6] Inst Theoret & Expt Phys, Moscow 117259, Russia

[7] Univ Bologna, I-40126 Bologna, Italy

[8] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy

[9] LIP, Lab Instrumentacao & Fis Expt Particulas, P-1000 Lisbon, Portugal

[10] Inst Super Tecn, P-1096 Lisbon, Portugal

[11] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy

[12] Univ Perugia, I-06100 Perugia, Italy

[13] MIT, Cambridge, MA 02139 USA

[14] Univ Geneva, DPNC, CH-1211 Geneva 4, Switzerland

[15] Ist Nazl Fis Nucl, Sez Milano, I-20133 Milan, Italy

[16] Univ Grenoble 1, CNRS, IN2P3, LPSC,Inst Polytech Grenoble, F-38026 Grenoble, France

[17] CNR, IROE, I-50125 Florence, Italy

[18] Natl Cent Univ, Chungli 32054, Taiwan

[19] Chinese Univ Sci & Technol, Hefei 230029, Anhui, Peoples R China

[20] Chinese Acad Sci, Inst High Energy Phys, Beijing 100039, Peoples R China

[21] Kurchatov Inst, Moscow 123182, Russia

[22] Ewha Womans Univ, Seoul 120750, South Korea

[23] Rhein Westfal TH Aachen, Inst Phys 3, D-52074 Aachen, Germany

[24] Ist Nazl Fis Nucl, Sez Pisa, I-56100 Pisa, Italy

[25] Univ Pisa, I-56100 Pisa, Italy

[26] Chinese Acad Sci, Inst Elect Engn, Beijing 100080, Peoples R China

[27] Aalto Univ, FIN-02540 Kylmala, Finland

[28] Univ Turku, FIN-20014 Turku, Finland

[29] Univ Savoie, LAPP, CNRS, IN2P3, F-74941 Annecy Le Vieux, France

[30] Rhein Westfal TH Aachen, Inst Phys 1, D-52074 Aachen, Germany

[31] Kyungpook Natl Univ, CHEP, Taegu 702701, South Korea

[32] Acad Sinica, Inst Phys, Nankang 11529, Taiwan

[33] Louisiana State Univ, Baton Rouge, LA 70803 USA

[34] Univ Politehn Bucuresti, Inst Microtechnol, R-76900 Bucharest, Romania

[35] Univ Bucharest, R-76900 Bucharest, Romania

[36] Johns Hopkins Univ, Baltimore, MD 21218 USA

[37] Univ Maryland, College Pk, MD 20742 USA

[38] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany

[39] Chinese Acad Sci, Ctr Space Sci & Applicat, Beijing 100080, Peoples R China

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 724卷 / 01期

基金：

中国国家自然科学基金;

关键词：

acceleration of particles; cosmic rays; nuclear reactions; nucleosynthesis; abundances; space vehicles; ISOTOPIC COMPOSITION; CHARGE COMPOSITION; SPACE-STATION; PROPAGATION; LITHIUM; GALAXY; ABUNDANCES; SECONDARY; CONSTRAINTS; BERYLLIUM;

D O I：

10.1088/0004-637X/724/1/329

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Measurement of the chemical and isotopic composition of cosmic rays is essential for the precise understanding of their propagation in the galaxy. While the model parameters are mainly determined using the B/C ratio, the study of extended sets of ratios can provide stronger constraints on the propagation models. In this paper, the relative abundances of light-nuclei lithium, beryllium, boron, and carbon are presented. The secondary-to-primary ratios Li/C, Be/C, and B/C have been measured in the kinetic energy range 0.35-45 GeV nucleon(-1). The isotopic ratio Li-7/Li-6 is also determined in the magnetic rigidity interval 2.5-6.3 GV. The secondary-to-secondary ratios Li/Be, Li/B, and Be/B are also reported. These measurements are based on the data collected by the Alpha Magnetic Spectrometer AMS-01 during the STS-91 space shuttle flight in 1998 June. Our experimental results are in substantial agreement with other measurements, where they exist. We describe our light-nuclei data with a diffusive-reacceleration model. A 10%-15% overproduction of Be is found in the model predictions and can be attributed to uncertainties in the production cross-section data.

引用

页码：329 / 340

页数：12

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