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: We report the properties of primary cosmic-ray sulfur (S) in the rigidity range 2.15 GV to 3.0 TV based on 0.38×10^{6} sulfur nuclei collected by the Alpha Magnetic Spectrometer experiment (AMS). We observed that above 90 GV the rigidity dependence of the S flux is identical to the rigidity dependence of Ne-Mg-Si fluxes, which is different from the rigidity dependence of the He-C-O-Fe fluxes. We found that, similar to N, Na, and Al cosmic rays, over the entire rigidity range, the traditional primary cosmic rays S, Ne, Mg, and C all have sizeable secondary components, and the S, Ne, and Mg fluxes are well described by the weighted sum of the primary silicon flux and the secondary fluorine flux, and the C flux is well described by the weighted sum of the primary oxygen flux and the secondary boron flux. The primary and secondary contributions of the traditional primary cosmic-ray fluxes of C, Ne, Mg, and S (even Z elements) are distinctly different from the primary and secondary contributions of the N, Na, and Al (odd Z elements) fluxes. The abundance ratio at the source for S/Si is 0.167±0.006, for Ne/Si is 0.833±0.025, for Mg/Si is 0.994±0.029, and for C/O is 0.836±0.025. These values are determined independent of cosmic-ray propagation.
Properties of Cosmic-Ray Sulfur and Determination of the Composition of Primary Cosmic-Ray Carbon, Neon, Magnesium, and Sulfur: Ten-Year Results from the Alpha Magnetic Spectrometer / Aguilar, M; Ali Cavasonza, L; Alpat, B; Ambrosi, G; Arruda, L; Attig, N; Bagwell, C; Barao, F; Barrin, L; Bartoloni, A; Başeğmez-du Pree, S; Battiston, R; Belyaev, N; Berdugo, J; Bertucci, B; Bindi, V; Bollweg, K; Bolster, J; Borchiellini, M; Borgia, B; Boschini, M J; Bourquin, M; Bueno, E F; Burger, J; Burger, W J; Cai, X D; Capell, M; Casaus, J; Castellini, G; Cervelli, F; Chang, Y H; Chen, G M; Chen, G R; Chen, H; Chen, H S; Chen, Y; Cheng, L; Chou, H Y; Chouridou, S; Choutko, V; Chung, C H; Clark, C; Coignet, G; Consolandi, C; Contin, A; Corti, C; Cui, Z; Dadzie, K; Dass, A; Delgado, C; Della Torre, S; Demirköz, M B; Derome, L; Di Falco, S; Di Felice, V; Díaz, C; Dimiccoli, F; von Doetinchem, P; Dong, F; Donnini, F; Duranti, M; Egorov, A; Eline, A; Faldi, F; Feng, J; Fiandrini, E; Fisher, P; Formato, V; Gámez, C; García-López, R J; Gargiulo, C; Gast, H; Gervasi, M; Giovacchini, F; Gómez-Coral, D M; Gong, J; Goy, C; Grabski, V; Grandi, D; Graziani, M; Guracho, A N; Haino, S; Han, K C; Hashmani, R K; He, Z H; Heber, B; Hsieh, T H; Hu, J Y; Huang, B W; Incagli, M; Jang, W Y; Jia, Yi; Jinchi, H; Karagöz, G; Khiali, B; Kim, G N; Kirn, Th; Kounina, O; Kounine, A; Koutsenko, V; Krasnopevtsev, D; Kuhlman, A; Kulemzin, A; La Vacca, G; Laudi, E; Laurenti, G; Lavecchia, G; Lazzizzera, I; Lee, H T; Lee, S C; Li, H L; Li, J Q; Li, M; Li, M; Li, Q; Li, Q; Li, Q Y; Li, S; Li, S L; Li, J H; Li, Z H; Liang, J; Liang, M J; Lin, C H; Lippert, T; Liu, J H; Lu, S Q; Lu, Y S; Luebelsmeyer, K; Luo, J Z; Luo, S D; Luo, Xi; Machate, F; Mañá, C; Marín, J; Marquardt, J; Martin, T; Martínez, G; Masi, N; Maurin, D; Medvedeva, T; Menchaca-Rocha, A; Meng, Q; Mikhailov, V V; Molero, M; Mott, P; Mussolin, L; Negrete, J; Nikonov, N; Nozzoli, F; Ocampo-Peleteiro, J; Oliva, A; Orcinha, M; Ottupara, M A; Palermo, M; Palmonari, F; Paniccia, M; Pashnin, A; Pauluzzi, M; Pensotti, S; Plyaskin, V; Poluianov, S; Qin, X; Qu, Z Y; Quadrani, L; Rancoita, P G; Rapin, D; Reina Conde, A; Robyn, E; Romaneehsen, L; Rozhkov, A; Rozza, D; Sagdeev, R; Schael, S; Schultz von Dratzig, A; Schwering, G; Seo, E S; Shan, B S; Siedenburg, T; Song, J W; Song, X J; Sonnabend, R; Strigari, L; Su, T; Sun, Q; Sun, Z T; Tacconi, M; Tang, X W; Tang, Z C; Tian, J; Tian, Y; Ting, Samuel C C; Ting, S M; Tomassetti, N; Torsti, J; Urban, T; Usoskin, I; Vagelli, V; Vainio, R; Valencia-Otero, M; Valente, E; Valtonen, E; Vázquez Acosta, M; Vecchi, M; Velasco, M; Vialle, J P; Wang, C X; Wang, L; Wang, L Q; Wang, N H; Wang, Q L; Wang, S; Wang, X; Wang, Yu; Wang, Z M; Wei, J; Weng, Z L; Wu, H; Wu, Y; Xiao, J N; Xiong, R Q; Xiong, X Z; Xu, W; Yan, Q; Yang, H T; Yang, Y; Yashin, I I; Yelland, A; Yi, H; You, Y H; Yu, Y M; Yu, Z Q; Zannoni, M; Zhang, C; Zhang, F; Zhang, F Z; Zhang, J; Zhang, J H; Zhang, Z; Zhao, F; Zheng, C; Zheng, Z M; Zhuang, H L; Zhukov, V; Zichichi, A; Zuccon, P. - In: PHYSICAL REVIEW LETTERS. - ISSN 0031-9007. - 130:21(2023), p. 211002. [10.1103/PhysRevLett.130.211002]
Properties of Cosmic-Ray Sulfur and Determination of the Composition of Primary Cosmic-Ray Carbon, Neon, Magnesium, and Sulfur: Ten-Year Results from the Alpha Magnetic Spectrometer
Aguilar, M;Ali Cavasonza, L;Alpat, B;Ambrosi, G;Arruda, L;Attig, N;Bagwell, C;Barao, F;Barrin, L;Bartoloni, A;Başeğmez-du Pree, S;Battiston, R;Belyaev, N;Berdugo, J;Bertucci, B;Bindi, V;Bollweg, K;Bolster, J;Borchiellini, M;Borgia, B;Boschini, M J;Bourquin, M;Bueno, E F;Burger, J;Burger, W J;Cai, X D;Capell, M;Casaus, J;Castellini, G;Cervelli, F;Chang, Y H;Chen, G M;Chen, G R;Chen, H;Chen, H S;Chen, Y;Cheng, L;Chou, H Y;Chouridou, S;Choutko, V;Chung, C H;Clark, C;Coignet, G;Consolandi, C;Contin, A;Corti, C;Cui, Z;Dadzie, K;Dass, A;Delgado, C;Della Torre, S;Demirköz, M B;Derome, L;Di Falco, S;Di Felice, V;Díaz, C;Dimiccoli, F;von Doetinchem, P;Dong, F;Donnini, F;Duranti, M;Egorov, A;Eline, A;Faldi, F;Feng, J;Fiandrini, E;Fisher, P;Formato, V;Gámez, C;García-López, R J;Gargiulo, C;Gast, H;Gervasi, M;Giovacchini, F;Gómez-Coral, D M;Gong, J;Goy, C;Grabski, V;Grandi, D;Graziani, M;Guracho, A N;Haino, S;Han, K C;Hashmani, R K;He, Z H;Heber, B;Hsieh, T H;Hu, J Y;Huang, B W;Incagli, M;Jang, W Y;Jia, Yi;Jinchi, H;Karagöz, G;Khiali, B;Kim, G N;Kirn, Th;Kounina, O;Kounine, A;Koutsenko, V;Krasnopevtsev, D;Kuhlman, A;Kulemzin, A;La Vacca, G;Laudi, E;Laurenti, G;LaVecchia, G;Lazzizzera, I;Lee, H T;Lee, S C;Li, H L;Li, J Q;Li, M;Li, M;Li, Q;Li, Q;Li, Q Y;Li, S;Li, S L;Li, J H;Li, Z H;Liang, J;Liang, M J;Lin, C H;Lippert, T;Liu, J H;Lu, S Q;Lu, Y S;Luebelsmeyer, K;Luo, J Z;Luo, S D;Luo, Xi;Machate, F;Mañá, C;Marín, J;Marquardt, J;Martin, T;Martínez, G;Masi, N;Maurin, D;Medvedeva, T;Menchaca-Rocha, A;Meng, Q;Mikhailov, V V;Molero, M;Mott, P;Mussolin, L;Negrete, J;Nikonov, N;Nozzoli, F;Ocampo-Peleteiro, J;Oliva, A;Orcinha, M;Ottupara, M A;Palermo, M;Palmonari, F;Paniccia, M;Pashnin, A;Pauluzzi, M;Pensotti, S;Plyaskin, V;Poluianov, S;Qin, X;Qu, Z Y;Quadrani, L;Rancoita, P G;Rapin, D;Reina Conde, A;Robyn, E;Romaneehsen, L;Rozhkov, A;Rozza, D;Sagdeev, R;Schael, S;Schultz von Dratzig, A;Schwering, G;Seo, E S;Shan, B S;Siedenburg, T;Song, J W;Song, X J;Sonnabend, R;Strigari, L;Su, T;Sun, Q;Sun, Z T;Tacconi, M;Tang, X W;Tang, Z C;Tian, J;Tian, Y;Ting, Samuel C C;Ting, S M;Tomassetti, N;Torsti, J;Urban, T;Usoskin, I;Vagelli, V;Vainio, R;Valencia-Otero, M;Valente, E;Valtonen, E;Vázquez Acosta, M;Vecchi, M;Velasco, M;Vialle, J P;Wang, C X;Wang, L;Wang, L Q;Wang, N H;Wang, Q L;Wang, S;Wang, X;Wang, Yu;Wang, Z M;Wei, J;Weng, Z L;Wu, H;Wu, Y;Xiao, J N;Xiong, R Q;Xiong, X Z;Xu, W;Yan, Q;Yang, H T;Yang, Y;Yashin, I I;Yelland, A;Yi, H;You, Y H;Yu, Y M;Yu, Z Q;Zannoni, M;Zhang, C;Zhang, F;Zhang, F Z;Zhang, J;Zhang, J H;Zhang, Z;Zhao, F;Zheng, C;Zheng, Z M;Zhuang, H L;Zhukov, V;Zichichi, A;Zuccon, P
2023-01-01
Abstract
: We report the properties of primary cosmic-ray sulfur (S) in the rigidity range 2.15 GV to 3.0 TV based on 0.38×10^{6} sulfur nuclei collected by the Alpha Magnetic Spectrometer experiment (AMS). We observed that above 90 GV the rigidity dependence of the S flux is identical to the rigidity dependence of Ne-Mg-Si fluxes, which is different from the rigidity dependence of the He-C-O-Fe fluxes. We found that, similar to N, Na, and Al cosmic rays, over the entire rigidity range, the traditional primary cosmic rays S, Ne, Mg, and C all have sizeable secondary components, and the S, Ne, and Mg fluxes are well described by the weighted sum of the primary silicon flux and the secondary fluorine flux, and the C flux is well described by the weighted sum of the primary oxygen flux and the secondary boron flux. The primary and secondary contributions of the traditional primary cosmic-ray fluxes of C, Ne, Mg, and S (even Z elements) are distinctly different from the primary and secondary contributions of the N, Na, and Al (odd Z elements) fluxes. The abundance ratio at the source for S/Si is 0.167±0.006, for Ne/Si is 0.833±0.025, for Mg/Si is 0.994±0.029, and for C/O is 0.836±0.025. These values are determined independent of cosmic-ray propagation.
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simulazione ASN
Il report seguente simula gli indicatori relativi alla propria produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione. La simulazione si basa sui dati IRIS e sugli indicatori bibliometrici alla data indicata e non tiene conto di eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori. La simulazione può differire dall'esito di un’eventuale domanda ASN sia per errori di catalogazione e/o dati mancanti in IRIS, sia per la variabilità dei dati bibliometrici nel tempo. Si consideri che Anvur calcola i valori degli indicatori all'ultima data utile per la presentazione delle domande.
La presente simulazione è stata realizzata sulla base delle specifiche raccolte sul tavolo ER del Focus Group IRIS coordinato dall’Università di Modena e Reggio Emilia e delle regole riportate nel DM 589/2018 e allegata Tabella A. Cineca, l’Università di Modena e Reggio Emilia e il Focus Group IRIS non si assumono alcuna responsabilità in merito all’uso che il diretto interessato o terzi faranno della simulazione. Si specifica inoltre che la simulazione contiene calcoli effettuati con dati e algoritmi di pubblico dominio e deve quindi essere considerata come un mero ausilio al calcolo svolgibile manualmente o con strumenti equivalenti.