Journal
PHYSICAL REVIEW LETTERS
Volume 113, Issue 12, Pages -Publisher
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevLett.113.121102
Keywords
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Funding
- NASA
- MIT, School of Science
- CAS, China
- NNSF, China
- MOST, China
- NLAA, China
- provincial government of Shandong, China
- provincial government of Jiangsu, China
- provincial government of Guangdong, China
- CNRS, France
- IN2P3, France
- CNES, France
- Enigmass, France
- ANR, France
- DLR, Germany
- INFN, Italy
- ASI, Italy
- CIEMAT, Spain
- CDTI, Spain
- SEIDI-MINECO, Spain
- CPAN, Spain
- Swiss National Science Foundation (SNSF), Switzerland
- Academia Sinica
- National Science Council (NSC)
- CERN
- ESA
- ASI Science Data Center (ASDC) [C/011/11/1]
- Centre national d'etudes spatiales, CNES
- Deutsches Zentrum fur Luft- und Raumfahrt, DLR
- JARA-HPC [JARA0052]
- Turkish Atomic Energy Authority, TAEK
- National Natural Science Foundation of China
- Italian Space Agency, ASI [ASI-INFN I/002/13/0]
- Ministry of Science and Technology
- CHEP, Kyungpook National University [NRF-2009-0080142, NRF-2012-010226]
- SEIDI
- CPAN
- Consejo Nacional de Ciencia y Tecnologia, CONACYT
- China Scholarship Council
- [NRF-2013-004883]
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Precision measurements by the Alpha Magnetic Spectrometer on the International Space Station of the primary cosmic-ray electron flux in the range 0.5 to 700 GeV and the positron flux in the range 0.5 to 500 GeV are presented. The electron flux and the positron flux each require a description beyond a single power-law spectrum. Both the electron flux and the positron flux change their behavior at similar to 30 GeV but the fluxes are significantly different in their magnitude and energy dependence. Between 20 and 200 GeV the positron spectral index is significantly harder than the electron spectral index. The determination of the differing behavior of the spectral indices versus energy is a new observation and provides important information on the origins of cosmic-ray electrons and positrons.
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