Precision Measurement of the Boron to Carbon Flux Ratio in Cosmic Rays from 1.9 GV to 2.6 TV with the Alpha Magnetic Spectrometer on the International Space Station

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dc.contributor.authorM. Aguilar
dc.contributor.authorL. Ali Cavasonza
dc.contributor.authorG. Ambrosi
dc.contributor.authorL. Arruda
dc.contributor.authorN. Attig
dc.contributor.authorS. Aupetit
dc.contributor.authorP. Azzarello
dc.contributor.authorA. Bachlechner
dc.contributor.authorF. Barao
dc.contributor.authorA. Barrau
dc.contributor.authorL. Barrin
dc.contributor.authorA. Bartoloni
dc.contributor.authorL. Basara
dc.contributor.authorS. Başeğmez-du Pree
dc.contributor.authorM. Battarbee
dc.contributor.authorR. Battiston
dc.contributor.authorU. Becker
dc.contributor.authorM. Behlmann
dc.contributor.authorB. Beischer
dc.contributor.authorJ. Berdugo
dc.contributor.authorB. Bertucci
dc.contributor.authorK. F. Bindel
dc.contributor.authorV. Bindi
dc.contributor.authorG. Boella
dc.contributor.authorW. de Boer
dc.contributor.authorK. Bollweg
dc.contributor.authorV. Bonnivard
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dc.contributor.authorM. J. Boschini
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dc.contributor.authorJ. Burger
dc.contributor.authorF. Cadoux
dc.contributor.authorX. D. Cai
dc.contributor.authorM. Capell
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dc.contributor.authorJ. Casaus
dc.contributor.authorG. Castellini
dc.contributor.authorF. Cervelli
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dc.contributor.authorY. H. Chang
dc.contributor.authorA. I. Chen
dc.contributor.authorG. M. Chen
dc.contributor.authorH. S. Chen
dc.contributor.authorL. Cheng
dc.contributor.authorH. Y. Chou
dc.contributor.authorE. Choumilov
dc.contributor.authorV. Choutko
dc.contributor.authorC. H. Chung
dc.contributor.authorC. Clark
dc.contributor.authorR. Clavero
dc.contributor.authorG. Coignet
dc.contributor.authorC. Consolandi
dc.contributor.authorA. Contin
dc.contributor.authorC. Corti
dc.contributor.authorW. Creus
dc.contributor.authorM. Crispoltoni
dc.contributor.authorZ. Cui
dc.contributor.authorY. M. Dai
dc.contributor.authorC. Delgado
dc.contributor.authorS. Della Torre
dc.contributor.authorO. Demakov
dc.contributor.authorM. B. Demirköz
dc.contributor.authorL. Derome
dc.contributor.authorS. Di Falco
dc.contributor.authorF. Dimiccoli
dc.contributor.authorC. Díaz
dc.contributor.authorP. von Doetinchem
dc.contributor.authorF. Dong
dc.contributor.authorF. Donnini
dc.contributor.authorM. Duranti
dc.contributor.authorD. D’Urso
dc.contributor.authorA. Egorov
dc.contributor.authorA. Eline
dc.contributor.authorT. Eronen
dc.contributor.authorJ. Feng
dc.contributor.authorE. Fiandrini
dc.contributor.authorE. Finch
dc.contributor.authorP. Fisher
dc.contributor.authorV. Formato
dc.contributor.authorY. Galaktionov
dc.contributor.authorG. Gallucci
dc.contributor.authorB. García
dc.contributor.authorR. J. García-López
dc.contributor.authorC. Gargiulo
dc.contributor.authorH. Gast
dc.contributor.authorI. Gebauer
dc.contributor.authorM. Gervasi
dc.contributor.authorA. Ghelfi
dc.contributor.authorF. Giovacchini
dc.contributor.authorP. Goglov
dc.contributor.authorD. M. Gómez-Coral
dc.contributor.authorJ. Gong
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dc.contributor.authorD. Grandi
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dc.contributor.authorK. C. Han
dc.contributor.authorZ. H. He
dc.contributor.authorM. Heil
dc.contributor.authorJ. Hoffman
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dc.contributor.authorH. Huang
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dc.contributor.authorTh. Kirn
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dc.contributor.authorM. S. Krafczyk
dc.contributor.authorG. La Vacca
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dc.contributor.authorG. Laurenti
dc.contributor.authorI. Lazzizzera
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dc.contributor.authorH. S. Li
dc.contributor.authorJ. Q. Li
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dc.contributor.authore J. Q. Li
dc.contributor.authorQ. Li
dc.contributor.authorT. X. Li
dc.contributor.authorW. Li
dc.contributor.authorY. Li
dc.contributor.authorZ. H. Li
dc.contributor.authorZ. Y. Li
dc.contributor.authorS. Lim
dc.contributor.authorC. H. Lin
dc.contributor.authorP. Lipari
dc.contributor.authorT. Lippert
dc.contributor.authorD. Liu
dc.contributor.authorHu Liu
dc.contributor.authorV. D. Lordello
dc.contributor.authorS. Q. Lu
dc.contributor.authorY. S. Lu
dc.contributor.authorK. Luebelsmeyer
dc.contributor.authorF. Luo
dc.contributor.authorJ. Z. Luo
dc.contributor.authorS. S. Lv
dc.contributor.authorF. Machate
dc.contributor.authorR. Majka
dc.contributor.authorC. Mañá
dc.contributor.authorJ. Marín
dc.contributor.authorT. Martin
dc.contributor.authorG. Martínez
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dc.contributor.authorD. Maurin
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dc.contributor.authorQ. Meng
dc.contributor.authorV. M. Mikuni
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dc.contributor.authorP. Saouter
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dc.contributor.authorA. Schulz von Dratzig
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dc.contributor.authorD. Son
dc.contributor.authorJ.W. Song
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dc.contributor.authorM. Tacconi
dc.contributor.authorX.W. Tang
dc.contributor.authorZ. C. Tang
dc.contributor.authorL. Tao
dc.contributor.authorD. Tescaro
dc.contributor.authorSamuel C. C. Ting
dc.contributor.authorS. M. Ting
dc.contributor.authorN. Tomassetti
dc.contributor.authorJ. Torsti
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dc.contributor.authorT. Urban
dc.contributor.authorV. Vagelli
dc.contributor.authorE. Valente
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dc.contributor.authorM. Vázquez Acosta
dc.contributor.authorM. Vecchi
dc.contributor.authorM. Velasco
dc.contributor.authorJ. P. Vialle
dc.contributor.authorV. Vitale
dc.contributor.authorS. Vitillo
dc.contributor.authorL. Q. Wang
dc.contributor.authorN. H. Wang
dc.contributor.authorQ. L. Wang
dc.contributor.authorX. Wang
dc.contributor.authorX. Q. Wang
dc.contributor.authorZ. X. Wang
dc.contributor.authorC. C. Wei
dc.contributor.authorZ. L. Weng
dc.contributor.authorK. Whitman
dc.contributor.authorJ. Wienkenhöver
dc.contributor.authorH. Wu
dc.contributor.authorX. Wu
dc.contributor.authorX. Xia
dc.contributor.authorR. Q. Xiong
dc.contributor.authorW. Xu
dc.contributor.authorQ. Yan
dc.contributor.authorJ. Yang
dc.contributor.authorM. Yang
dc.contributor.authorY. Yang
dc.contributor.authorH. Yi
dc.contributor.authorY. J. Yu
dc.contributor.authorZ. Q. Yu
dc.contributor.authorS. Zeissler
dc.contributor.authorC. Zhang
dc.contributor.authorJ. Zhang
dc.contributor.authorJ. H. Zhang
dc.contributor.authorS. D. Zhang
dc.contributor.authorS.W. Zhang
dc.contributor.authorZ. Zhang
dc.contributor.authorZ. M. Zheng
dc.contributor.authorZ. Q. Zhu
dc.contributor.authorH. L. Zhuang
dc.contributor.authorV. Zhukov
dc.contributor.authorA. Zichichi
dc.contributor.authorN. Zimmermann
dc.contributor.authorand P. Zuccon
dc.contributor.organizationfi=avaruustutkimuslaboratorio|en=Space Research Laboratory|
dc.contributor.organization-code1.2.246.10.2458963.20.47833719389
dc.contributor.organization-code2606702
dc.converis.publication-id18606053
dc.converis.urlhttps://research.utu.fi/converis/portal/Publication/18606053
dc.date.accessioned2022-10-28T14:07:45Z
dc.date.available2022-10-28T14:07:45Z
dc.description.abstract<p>Knowledge of the rigidity dependence of the boron to carbon flux ratio (B/C) is important in understanding the propagation of cosmic rays. The precise measurement of the B/C ratio from 1.9 GV to 2.6 TV, based on 2.3 million boron and 8.3 million carbon nuclei collected by AMS during the first 5 years of operation, is presented. The detailed variation with rigidity of the B/C spectral index is reported for the first time. The B/C ratio does not show any significant structures in contrast to many cosmic ray models that require such structures at high rigidities. Remarkably, above 65 GV, the B/C ratio is well described by a single power law R<sup>Δ</sup> with index Δ = −0.333 +/- 0.014(fit) +/- 0.005(syst), in good agreement with the Kolmogorov theory of turbulence which predicts Δ = −1/3 asymptotically.</p>
dc.format.pagerange231102-1
dc.format.pagerange231102-8
dc.identifier.eissn1079-7114
dc.identifier.jour-issn0031-9007
dc.identifier.olddbid186434
dc.identifier.oldhandle10024/169528
dc.identifier.urihttps://www.utupub.fi/handle/11111/38520
dc.identifier.urlhttp://journals.aps.org/prl/abstract/10.1103/PhysRevLett.117.231102
dc.identifier.urnURN:NBN:fi-fe2021042716448
dc.language.isoen
dc.okm.affiliatedauthorEronen, Timo
dc.okm.affiliatedauthorTorsti, Jarmo
dc.okm.affiliatedauthorValtonen, Eino
dc.okm.discipline114 Physical sciencesen_GB
dc.okm.discipline114 Fysiikkafi_FI
dc.okm.internationalcopublicationinternational co-publication
dc.okm.internationalityInternational publication
dc.okm.typeA1 ScientificArticle
dc.publisherAmerican Physical Society
dc.publisher.countryUnited Statesen_GB
dc.publisher.countryYhdysvallat (USA)fi_FI
dc.publisher.country-codeUS
dc.relation.articlenumber231102
dc.relation.doi10.1103/PhysRevLett.117.231102
dc.relation.ispartofjournalPhysical Review Letters
dc.relation.issue23
dc.relation.volume117
dc.source.identifierhttps://www.utupub.fi/handle/10024/169528
dc.titlePrecision Measurement of the Boron to Carbon Flux Ratio in Cosmic Rays from 1.9 GV to 2.6 TV with the Alpha Magnetic Spectrometer on the International Space Station
dc.year.issued2016

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