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., … AMS Collaboration. (2023). 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. Physical Review Letters, 130(21), 211002. https://doi.org/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
|Author:||Aguilar, M.1; Cavasonza, L. Ali2,3; Alpat, B.4;|
1Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid 28040, Spain.
2Rhein Westfal TH Aachen, Phys Inst, D-52056 Aachen, Germany.
3Rhein Westfal TH Aachen, JARA FAME, D-52056 Aachen, Germany.
4INFN, Sez Perugia, I-06100 Perugia, Italy.
5Lab Instrumentacao & Fis Expt Particulas LIP, P-1649003 Lisbon, Portugal.
6Res Ctr Julich, Julich Supercomp Ctr, D-52425 Julich, Germany.
7Res Ctr Julich, JARA FAME, D-52425 Julich, Germany.
8MIT, Cambridge, MA 02139 USA.
9European Org Nucl Res CERN, CH-1211 Geneva 23, Switzerland.
10INFN, Sez Roma 1, I-00185 Rome, Italy.
11Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
12Nikhef, NL-1098 XG Amsterdam, Netherlands.
13INFN, TIFPA, I-38123 Trento, Italy.
14Univ Trento, I-38123 Trento, Italy.
15Univ Perugia, I-06100 Perugia, Italy.
16Univ Hawaii, Phys & Astron Dept, Honolulu, HI 96822 USA.
17NASA, Johnson Space Ctr JSC, Houston, TX 77058 USA.
18INFN, Sez Milano Bicocca, I-20126 Milan, Italy.
19Univ Geneva, DPNC, CH-1211 Geneva 4, Switzerland.
20CNR IROE, I-50125 Florence, Italy.
21INFN, Sez Pisa, I-56100 Pisa, Italy.
22Acad Sinica, Inst Phys, Taipei 11529, Taiwan.
23Chinese Acad Sci, Inst High Energy Phys IHEP, Beijing 100049, Peoples R China.
24Univ Chinese Acad Sci UCAS, Beijing 100049, Peoples R China.
25Shandong Inst Adv Technol SDIAT, Jinan 250100, Shandong, Peoples R China.
26Zhejiang Univ ZJU, Hangzhou 310058, Peoples R China.
27Univ Savoie Mont Blanc, Univ Grenoble Alpes, CNRS, LAPP IN2P3, F-74000 Annecy, France.
28INFN, Sez Bologna, I-40126 Bologna, Italy.
29Univ Bologna, I-40126 Bologna, Italy.
30Shandong Univ SDU, Jinan 250100, Shandong, Peoples R China.
31Middle East Tech Univ METU, Dept Phys, TR-06800 Ankara, Turkiye.
32Univ Grenoble Alpes, CNRS, Grenoble INP, LPSC IN2P3, F-38000 Grenoble, France.
33INFN, Sez Roma Tor Vergata, I-00133 Rome, Italy.
34Southeast Univ SEU, Nanjing 210096, Peoples R China.
35Sun Yat Sen Univ SYSU, Guangzhou 510275, Peoples R China.
36Inst Astrofis Canarias IAC, San Cristobal la Laguna 38205, Tenerife, Spain.
37Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain.
38Univ Milano Bicocca, I-20126 Milan, Italy.
39Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 01000, Mexico.
40Natl Chung Shan Inst Sci & Technol NCSIST, Tao Yuan 32546, Taiwan.
41Christian Alberts Univ Kiel, Inst Expt & Angew Phys, D-24118 Kiel, Germany.
42Kyungpook Natl Univ, CHEP, Daegu 41566, South Korea.
43Acad Sinica Grid Ctr ASGC, Taipei 11529, Taiwan.
44Chinese Acad Sci, Inst Elect Engn IEE, Beijing 100190, Peoples R China.
45NRNU, MEPhI Moscow Engn Phys Inst, Moscow 115409, Russia.
46Sodankylä Geophysical Observatory and Space Physics and Astronomy Research Unit, University of Oulu, 90014 Oulu, Finland
47Univ Maryland, East West Ctr Space Sci, College Pk, MD 20742 USA.
48Univ Maryland, IPST, College Pk, MD 20742 USA.
49Beihang Univ BUAA, Beijing 100191, Peoples R China.
50IRCCS Azienda Osped Univ Bologna, Bologna, Italy.
51Univ Turku, Dept Phys & Astron, Space Res Lab, Turku 20014, Finland.
52Physics Department and Center for High Energy and High Field Physics, National Central University (NCU), Tao Yuan 32054, Taiwan
53Agenzia Spaziale Italiana ASI, I-00133 Rome, Italy.
54Natl Cheng Kung Univ, Tainan 70101, Taiwan.
|Online Access:||PDF Full Text (PDF, 0.6 MB)|
|Persistent link:|| http://urn.fi/urn:nbn:fi-fe20230921135058
American Physical Society,
|Publish Date:|| 2023-09-21
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 x 10⁶ 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.
Physical review letters
|Type of Publication:||
A1 Journal article – refereed
|Field of Science:||
115 Astronomy and space science
We are grateful for the support of Glen Crawford of the DOE including resources from the National Energy Research Scientific Computing Center under Contract No. DE-AC02-05CH11231. We gratefully acknowledge the strong support from CERN including Fabiola Gianotti, and the CERN IT department including Bernd Panzer-Steindel. We also acknowledge the continuous support from MIT and its School of Science, Nergis Mavalvala, and the Laboratory for Nuclear Science, Boleslaw Wyslouch. Research supported by Chinese Academy of Sciences, Institute of High Energy Physics, Institute of Electrical Engineering, China Academy of Space Technology, National Natural Science Foundation (NSFC) , and Ministry of Science and Technology, National Key R & amp;D Program Grants No. 2022YFA1604802 and No. 2022YFA1604803, NSFC Grant No. 12275158, the China Scholarship Council, the provincial governments of Shandong, Jiangsu, Guangdong, Shandong University, and the Shandong Institute of Advanced Technology, China; the Academy of Finland, Project No. 321882, Finland; CNRS/IN2P3 and CNES, France; DLR under Grants No. 50OO1803 and computing support on the JARA Partition of the RWTH Aachen supercomputer, Germany; INFN and ASI under ASI-INFN Agreements No. 2019-19-HH.0, its amendments, and No. 2021-43-HH.0 and ASI-University of Perugia Agreement No. 2019-2-HH.0, Italy; CHEP and NRF under Grant No. NRF-2018R1A6A1A06024970 at Kyungpook National University, Korea; the Consejo Nacional de Ciencia y Tecnologia and UNAM, Mexico; NWO under Grant No. 680-1-004, Netherlands; FCT under Grant No. CERN/FIS-PAR/0013/2019, Portugal; the Ministry of Science and Higher Education under Project No. 0723-2020-0040, Russia; CIEMAT, IAC, CDTI, and SEIDI-MINECO under Grants No. PID2019-107988 GB-C21/C22, and No. CEX2019-000920-S, Spain; the Fondation Dr. Manfred Steuer, Switzerland; Academia Sinica, the National Science and Technology Council (NSTC) , formerly the Ministry of Science and Technology (MOST) , under Grants No. 111-2123-M-001-004 and No. 111-2112-M-006-029, High Education Sprout Project by the Ministry of Education at National Cheng Kung University, former Presidents of Academia Sinica Yuan-Tseh Lee and Chi-Huey Wong and former Ministers of NSTC (formerly MOST) Maw-Kuen Wu and Luo-Chuan Lee, Taiwan; the Turkish Energy, Nuclear and Mineral Research Agency (TENMAK) under Grant No. 2020TAEK (CERN) A5.H1.F5-26, Turkey; and NSF Grant No. 2013228 and ANSWERS proposals No. 2149809, No. 2149810, and No. 2149811, LWS NASA Grant/Cooperative Agreement No. 80NSSC20K1819, and NASA Grant No. 80NSSC21K1392, USA.
|Academy of Finland Grant Number:||
321882 (Academy of Finland Funding decision)
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