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 7Li/6Li 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.
| 原文 | ???core.languages.en_GB??? |
|---|---|
| 頁（從 - 到） | 329-340 |
| 頁數 | 12 |
| 期刊 | Astrophysical Journal |
| 卷 | 724 |
| 發行號 | 1 |
| DOIs | |
| 出版狀態 | 已出版 - 20 11月 2010 |
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Relative composition and energy spectra of light nuclei in cosmic rays : Results from AMS-01. / Aguilar, M.; Alcaraz, J.; Allaby, J.; Alpat, B.; Ambrosi, G.; Anderhub, H.; Ao, L.; Arefiev, A.; Arruda, L.; Azzarello, P.; Basile, M.; Barao, F.; Barreira, G.; Bartoloni, A.; Battiston, R.; Becker, R.; Becker, U.; Bellagamba, L.; Béné, P.; Berdugo, J.; Berges, P.; Bertucci, B.; Biland, A.; Bindi, V.; Boella, G.; Boschini, M.; Bourquin, M.; Bruni, G.; Buénerd, M.; Burger, J. D.; Burger, W. J.; Cai, X. D.; Cannarsa, P.; Capell, M.; Casadei, D.; Casaus, J.; Castellini, G.; Cernuda, I.; Chang, Y. H.; Chen, H. F.; Chen, H. S.; Chen, Z. G.; Chernoplekov, N. A.; Chiueh, T. H.; Choi, Y. Y.; Cindolo, F.; Commichau, V.; Contin, A.; Cortina-Gil, E.; Crespo, D.; Cristinziani, M.; Dai, T. S.; Dela Guia, C.; Delgado, C.; Di Falco, S.; Djambazov, L.; D'Antone, I.; Dong, Z. R.; Duranti, M.; Engelberg, J.; Eppling, F. J.; Eronen, T.; Extermann, P.; Favier, J.; Fiandrini, E.; Fisher, P. H.; Flügge, G.; Fouque, N.; Galaktionov, Y.; Gervasi, M.; Giovacchini, F.; Giusti, P.; Grandi, D.; Grimm, O.; Gu, W. Q.; Haino, S.; Hangarter, K.; Hasan, A.; Hermel, V.; Hofer, H.; Hungerford, W.; Ionica, M.; Jongmanns, M.; Karlamaa, K.; Karpinski, W.; Kenney, G.; Kim, D. H.; Kim, G. N.; Kim, K. S.; Kirn, T.; Klimentov, A.; Kossakowski, R.; Kounine, A.; Koutsenko, V.; Kraeber, M.; Laborie, G.; Laitinen, T.; Lamanna, G.; Laurenti, G.; Lebedev, A.; Lechanoine-Leluc, C.; Lee, M. W.; Lee, S. C.; Levi, G.; Lin, C. H.; Liu, H. T.; Lu, G.; Lu, Y. S.; Lübelsmeyer, K.; Luckey, D.; Lustermann, W.; Maña, C.; Margotti, A.; Mayet, F.; McNeil, R. R.; Menichelli, M.; Mihul, A.; Mujunen, A.; Oliva, A.; Palmonari, F.; Park, H. B.; Park, W. H.; Pauluzzi, M.; Pauss, F.; Pereira, R.; Perrin, E.; Pevsner, A.; Pilo, F.; Pimenta, M.; Plyaskin, V.; Pojidaev, V.; Pohl, M.; Produit, N.; Quadrani, L.; Rancoita, P. G.; Rapin, D.; Ren, D.; Ren, Z.; Ribordy, M.; Richeux, J. P.; Riihonen, E.; Ritakari, J.; Ro, S.; Roeser, U.; Sagdeev, R.; Santos, D.; Sartorelli, G.; Sbarra, C.; Schael, S.; Von Dratzig, A. Schultz; Schwering, G.; Seo, E. S.; Shin, J. W.; Shoumilov, E.; Shoutko, V.; Siedenburg, T.; Siedling, R.; Son, D.; Song, T.; Spada, F. R.; Spinella, F.; Steuer, M.; Sun, G. S.; Suter, H.; Tang, X. W.; Ting, Samuel C.C.; Ting, S. M.; Tomassetti, N.; Tornikoski, M.; Torsti, J.; Trümper, J.; Ulbricht, J.; Urpo, S.; Valtonen, E.; Vandenhirtz, J.; Velikhov, E.; Verlaat, B.; Vetlitsky, I.; Vezzu, F.; Vialle, J. P.; Viertel, G.; Vité, D.; Von Gunten, H.; Wicki, S. Waldmeier; Wallraff, W.; Wang, J. Z.; Wiik, K.; Williams, C.; Wu, S. X.; Xia, P. C.; Xu, S.; Xu, Z. Z.; Yan, J. L.; Yan, L. G.; Yang, C. G.; Yang, J.; Yang, M.; Ye, S. W.; Zhang, H. Y.; Zhang, Z. P.; Zhao, D. X.; Zhou, F.; Zhou, Y.; Zhu, G. Y.; Zhu, W. Z.; Zhuang, H. L.; Zichichi, A.; Zimmermann, B.; Zuccon, P.
於: Astrophysical Journal, 卷 724, 編號 1, 20.11.2010, p. 329-340.研究成果: 雜誌貢獻 › 期刊論文 › 同行評審
TY - JOUR
T1 - Relative composition and energy spectra of light nuclei in cosmic rays
T2 - Results from AMS-01
AU - Aguilar, M.
AU - Alcaraz, J.
AU - Allaby, J.
AU - Alpat, B.
AU - Ambrosi, G.
AU - Anderhub, H.
AU - Ao, L.
AU - Arefiev, A.
AU - Arruda, L.
AU - Azzarello, P.
AU - Basile, M.
AU - Barao, F.
AU - Barreira, G.
AU - Bartoloni, A.
AU - Battiston, R.
AU - Becker, R.
AU - Becker, U.
AU - Bellagamba, L.
AU - Béné, P.
AU - Berdugo, J.
AU - Berges, P.
AU - Bertucci, B.
AU - Biland, A.
AU - Bindi, V.
AU - Boella, G.
AU - Boschini, M.
AU - Bourquin, M.
AU - Bruni, G.
AU - Buénerd, M.
AU - Burger, J. D.
AU - Burger, W. J.
AU - Cai, X. D.
AU - Cannarsa, P.
AU - Capell, M.
AU - Casadei, D.
AU - Casaus, J.
AU - Castellini, G.
AU - Cernuda, I.
AU - Chang, Y. H.
AU - Chen, H. F.
AU - Chen, H. S.
AU - Chen, Z. G.
AU - Chernoplekov, N. A.
AU - Chiueh, T. H.
AU - Choi, Y. Y.
AU - Cindolo, F.
AU - Commichau, V.
AU - Contin, A.
AU - Cortina-Gil, E.
AU - Crespo, D.
AU - Cristinziani, M.
AU - Dai, T. S.
AU - Dela Guia, C.
AU - Delgado, C.
AU - Di Falco, S.
AU - Djambazov, L.
AU - D'Antone, I.
AU - Dong, Z. R.
AU - Duranti, M.
AU - Engelberg, J.
AU - Eppling, F. J.
AU - Eronen, T.
AU - Extermann, P.
AU - Favier, J.
AU - Fiandrini, E.
AU - Fisher, P. H.
AU - Flügge, G.
AU - Fouque, N.
AU - Galaktionov, Y.
AU - Gervasi, M.
AU - Giovacchini, F.
AU - Giusti, P.
AU - Grandi, D.
AU - Grimm, O.
AU - Gu, W. Q.
AU - Haino, S.
AU - Hangarter, K.
AU - Hasan, A.
AU - Hermel, V.
AU - Hofer, H.
AU - Hungerford, W.
AU - Ionica, M.
AU - Jongmanns, M.
AU - Karlamaa, K.
AU - Karpinski, W.
AU - Kenney, G.
AU - Kim, D. H.
AU - Kim, G. N.
AU - Kim, K. S.
AU - Kirn, T.
AU - Klimentov, A.
AU - Kossakowski, R.
AU - Kounine, A.
AU - Koutsenko, V.
AU - Kraeber, M.
AU - Laborie, G.
AU - Laitinen, T.
AU - Lamanna, G.
AU - Laurenti, G.
AU - Lebedev, A.
AU - Lechanoine-Leluc, C.
AU - Lee, M. W.
AU - Lee, S. C.
AU - Levi, G.
AU - Lin, C. H.
AU - Liu, H. T.
AU - Lu, G.
AU - Lu, Y. S.
AU - Lübelsmeyer, K.
AU - Luckey, D.
AU - Lustermann, W.
AU - Maña, C.
AU - Margotti, A.
AU - Mayet, F.
AU - McNeil, R. R.
AU - Menichelli, M.
AU - Mihul, A.
AU - Mujunen, A.
AU - Oliva, A.
AU - Palmonari, F.
AU - Park, H. B.
AU - Park, W. H.
AU - Pauluzzi, M.
AU - Pauss, F.
AU - Pereira, R.
AU - Perrin, E.
AU - Pevsner, A.
AU - Pilo, F.
AU - Pimenta, M.
AU - Plyaskin, V.
AU - Pojidaev, V.
AU - Pohl, M.
AU - Produit, N.
AU - Quadrani, L.
AU - Rancoita, P. G.
AU - Rapin, D.
AU - Ren, D.
AU - Ren, Z.
AU - Ribordy, M.
AU - Richeux, J. P.
AU - Riihonen, E.
AU - Ritakari, J.
AU - Ro, S.
AU - Roeser, U.
AU - Sagdeev, R.
AU - Santos, D.
AU - Sartorelli, G.
AU - Sbarra, C.
AU - Schael, S.
AU - Von Dratzig, A. Schultz
AU - Schwering, G.
AU - Seo, E. S.
AU - Shin, J. W.
AU - Shoumilov, E.
AU - Shoutko, V.
AU - Siedenburg, T.
AU - Siedling, R.
AU - Son, D.
AU - Song, T.
AU - Spada, F. R.
AU - Spinella, F.
AU - Steuer, M.
AU - Sun, G. S.
AU - Suter, H.
AU - Tang, X. W.
AU - Ting, Samuel C.C.
AU - Ting, S. M.
AU - Tomassetti, N.
AU - Tornikoski, M.
AU - Torsti, J.
AU - Trümper, J.
AU - Ulbricht, J.
AU - Urpo, S.
AU - Valtonen, E.
AU - Vandenhirtz, J.
AU - Velikhov, E.
AU - Verlaat, B.
AU - Vetlitsky, I.
AU - Vezzu, F.
AU - Vialle, J. P.
AU - Viertel, G.
AU - Vité, D.
AU - Von Gunten, H.
AU - Wicki, S. Waldmeier
AU - Wallraff, W.
AU - Wang, J. Z.
AU - Wiik, K.
AU - Williams, C.
AU - Wu, S. X.
AU - Xia, P. C.
AU - Xu, S.
AU - Xu, Z. Z.
AU - Yan, J. L.
AU - Yan, L. G.
AU - Yang, C. G.
AU - Yang, J.
AU - Yang, M.
AU - Ye, S. W.
AU - Zhang, H. Y.
AU - Zhang, Z. P.
AU - Zhao, D. X.
AU - Zhou, F.
AU - Zhou, Y.
AU - Zhu, G. Y.
AU - Zhu, W. Z.
AU - Zhuang, H. L.
AU - Zichichi, A.
AU - Zimmermann, B.
AU - Zuccon, P.
PY - 2010/11/20
Y1 - 2010/11/20
N2 - 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 7Li/6Li 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.
AB - 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 7Li/6Li 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.
KW - Acceleration of particles
KW - Cosmic rays, nuclear reactions, nucleosynthesis, abundances
KW - Space vehicles
UR - http://www.scopus.com/inward/record.url?scp=78650108170&partnerID=8YFLogxK
U2 - 10.1088/0004-637X/724/1/329
DO - 10.1088/0004-637X/724/1/329
M3 - 期刊論文
AN - SCOPUS:78650108170
VL - 724
SP - 329
EP - 340
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
ER -