Leptons in near earth orbit

Alcaraz, J.; Alpat, B.; Ambrosi, G.; Anderhub, H.; Ao, L.; Arefiev, A.; Azzarello, P.; Babucci, E.; Baldini, Luca; Basile, M.; Barancourt, D.; Barão, F.; Barbier, G.; Barreira, G.; Battiston, R.; Becker, R. H.; Becker, U.; Bellagamba, L.; Béné, P.; Berdugo, J.; Berges, P.; Bertucci, B.; Biland, A.; Bizzaglia, S.; Blasko, S.; Boella, G.; Boschini, M.; Bourquin, M.; Brocco, L.; Bruni, G.; Buénerd, M.; Burger, J. D.; Burger, W. J.; Cai, Xudong; Camps, C.; Cannarsa, Piermarco; Capell, M.; Casadei, D.; Casaus, J.; Castellini, G.; Cecchi, C.; Chang, Y. H.; Chen, H.F.; Chen, H.S.; Chen, Z.G.; Chernoplekov, N. A.; Chiueh, Tzihong; Chuang, Yao-Li; Cindolo, F.; Commichau, V.; Contin, A.; Crespo, Paulo; Cristinziani, M.; Cunha, J. Pinto da; Dai, T.; Deus, J. Dias de; Dinu, N.; Djambazov, L.; D’Antone, I.; Dong, Zhiwen; Emonet, P.; Engelberg, J.; Eppling, F. J.; Eronen, T.; Esposito, G.; Extermann, P.; Favier, Jean; Fiandrini, E.; Fisher, P. H.; Fluegge, G.; Fouque, N.; Galaktionov, Yu.; Gervasi, M.; Giusti, P.; Grandi, D.; Grimm, O.; Gu, W.; Hangarter, K.; Hasan, A.; Hermel, V.; Hofer, H.; Huang, M. A.; Hungerford, W.; Ionica, M.; Ionica, R.; Jongmanns, M.; Karlamaa, K.; Karpiński, W.; Kenney, G.; Kenny, J. M.; Kim, W.; Klimentov, A.; Kossakowski, R.; Koutsenko, V.; Kraeber, M.; Laborie, G.; Laitinen, Timo; Lamanna, G.; Laurenti, G.; Lebedev, A.; Lee, S.C.; Levi, G.; Levtchenko, P.; Liu, C.L.; Liu, H.T.; Lopes, I.; Lu, Gangcheng; Lu, Yao; Lübelsmeyer, K.; Luckey, D.; Lustermann, W.; Mañá, C.; Margotti, A.; Mayet, F.; McNeil, R. R.; Meillon, Brigitte; Menichelli, M.; Mihul, A.; Mourão, A.; Mujunen, Ari; Palmonari, F.; Papi, Alberto; Park, I.H.; Pauluzzi, M.; Pauß, F.; Perrin, E.; Pesci, A.; Pevsner, A.; Pimenta, M.; Plyaskin, V.; Pojidaev, V.; Postolache, V.; Produit, N.; Rancoita, P.G.; Rapin, D.; Raupach, F.; Ren, D.; Ren, Zhiyuan; Ribordy, M.; Richeux, J.P.; Riihonen, E.; Ritakari, Jouko; Roeser, U.; Roissin, C.; Sagdeev, R. Z.; Sartorelli, G.; Dratzig, A. Schultz von; Schwering, G.; Scolieri, G.; Seo, E. S.; Shoutko, V.; Shoumilov, E.; Siedling, R.; Son, D. C.; Song, Tao; Steuer, M.; Sun, G.S.; Suter, H.; Tang, X.; Ting, Samuel C.C.; Ting, S. M.; Tornikoski, M.; Torsti, J.; Trümper, J.; Ulbricht, J.; Urpo, S.; Usoskin, Ilya; Валтонен, Э.; Vandenhirtz, J.; Velcea, F.; Velikhov, E. P.; Verlaat, B.; Vetlitsky, I.; Vezzu, F.; Vialle, J. P.; Viertel, G.; Vitè, Davide; Gunten, H. von; Wicki, S. Waldmeier; Wallraff, W.; Wang, B.C.; Wang, J.Z.; Wang, Y.H.; Wiik, K.; Williams, C.; Wu, S. X.; Xia, Pan; Yan, J.L.; Yan, L.G.; Yang, Changgen; Yang, Min; Ye, S.W.; Yeh, P.; Xu, Zun-Lei; Zhang, H.Y.; Zhang, Z.P.; Zhao, D.X.; Zhu, G.Y.; Zhu, Wei; Zhuang, H. L.; Zichichi, A.; Zimmermann, B.

doi:10.1016/s0370-2693(00)00588-8

Cited by 254 publications

(152 citation statements)

References 12 publications

(7 reference statements)

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“…4.38. This region matches that from which the second proton ux and second positron ux originate [37,40]. Within the statistics, 3 He is equally predominate in events from both the "short-" and "long-lived" classes.…”

Section: Analysis Of the Helium Second Spectrumsupporting

confidence: 65%

“…To understand the origin of these events, the trajectories have been traced both backward and forward from their incident angle, location and momentum through the Earth's magnetic ÿeld, following the same procedure as described in [37,40]. All events were found to originate in the atmosphere.…”

Section: Analysis Of the Helium Second Spectrummentioning

confidence: 99%

“…In this report we present the data collected during the ight to study the cosmic ray proton spectrum from kinetic energies of 0.1-200 GeV [37,38], the helium spectrum over the kinetic energy range 0.1-100 GeV=nucleon [39] and the spectra of electrons and positrons over the respective kinetic energy ranges of 0.2-30 GeV and 0.2-3 GeV [40], the latter range being limited by the proton background. Antiproton and deuteron spectra were measured from 0.2 to 4 GeV and from 0.09 to 0:85 GeV=nucleon.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The Alpha Magnetic Spectrometer (AMS) on the International Space Station: Part I – results from the test flight on the space shuttle

Aguilar¹,

Alcaraz²,

et al. 2002

Self Cite

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Section: Analysis Of the Helium Second Spectrumsupporting

confidence: 65%

Section: Analysis Of the Helium Second Spectrummentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The Alpha Magnetic Spectrometer (AMS) on the International Space Station: Part I – results from the test flight on the space shuttle

Aguilar¹,

Alcaraz²,

et al. 2002

Self Cite

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“…Since τ E determines the positron propagation scale, the related Table 1. Data are taken from CAPRICE (Boezio et al 2000), HEAT (Barwick et al 1997), AMS (Aguilar et al 2007;Alcaraz et al 2000) and MASS (Grimani et al 2002). uncertainties should have a far stronger effect on the primary contributions with a far greater spatial (or time) dependency, such as for instance nearby astrophysical or exotic point sources.…”

Section: Energy Lossesmentioning

confidence: 99%

Galactic secondary positron flux at the Earth

Delahaye

Lineros²,

Donato³

et al. 2009

A&A

217

308

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Context. Secondary positrons are produced by spallation of cosmic rays within the interstellar gas. Measurements have been typically expressed in terms of the positron fraction, which exhibits an increase above 10 GeV. Many scenarios have been proposed to explain this feature, among them some additional primary positrons originating from dark matter annihilation in the Galaxy. Aims. The PAMELA satellite has provided high quality data that has enabled high accuracy statistical analyses to be made, showing that the increase in the positron fraction extends up to about 100 GeV. It is therefore of paramount importance to constrain theoretically the expected secondary positron flux to interpret the observations in an accurate way. Methods. We focus on calculating the secondary positron flux by using and comparing different up-to-date nuclear cross-sections and by considering an independent model of cosmic ray propagation. We carefully study the origins of the theoretical uncertainties in the positron flux. Results. We find the secondary positron flux to be reproduced well by the available observations, and to have theoretical uncertainties that we quantify to be as large as about one order of magnitude. We also discuss the positron fraction issue and find that our predictions may be consistent with the data taken before PAMELA. For PAMELA data, we find that an excess is probably present after considering uncertainties in the positron flux, although its amplitude depends strongly on the assumptions made in relation to the electron flux. By fitting the current electron data, we show that when considering a soft electron spectrum, the amplitude of the excess might be far lower than usually claimed. Conclusions. We provide fresh insights that may help to explain the positron data with or without new physical model ingredients. PAMELA observations and the forthcoming AMS-02 mission will allow stronger constraints to be aplaced on the cosmic-ray transport parameters, and are likely to reduce drastically the theoretical uncertainties.

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“…To select only primary cosmic rays, the measured rigidity is required to exceed the maximum geomagnetic cutoff by a factor of 1.2 for either positive or negative particles within the AMS field of view. The cutoff is calculated by backtracing [16,27] using the most recent IGRF geomagnetic model [28].…”

mentioning

confidence: 99%

Antiproton Flux, Antiproton-to-Proton Flux Ratio, and Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station

Aguilar¹,

Cavasonza²,

Alpat³

et al. 2016

Phys. Rev. Lett.

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468

560

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International audienceA precision measurement by AMS of the antiproton flux and the antiproton-to-proton flux ratio inprimary cosmic rays in the absolute rigidity range from 1 to 450 GV is presented based on 3.49 × 105antiproton events and 2.42 × 109 proton events. The fluxes and flux ratios of charged elementary particlesin cosmic rays are also presented. In the absolute rigidity range ∼60 to ∼500 GV, the antiproton ¯p, protonp, and positron eþ fluxes are found to have nearly identical rigidity dependence and the electron e− fluxexhibits a different rigidity dependence. Below 60 GV, the ( ¯ p=p), ( ¯ p=eþ), and (p=eþ) flux ratios eachreaches a maximum. From ∼60 to ∼500 GV, the ( ¯ p=p), ( ¯ p=eþ), and (p=eþ) flux ratios show no rigiditydependence. These are new observations of the properties of elementary particles in the cosmos

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Leptons in near earth orbit

Cited by 254 publications

References 12 publications

The Alpha Magnetic Spectrometer (AMS) on the International Space Station: Part I – results from the test flight on the space shuttle

The Alpha Magnetic Spectrometer (AMS) on the International Space Station: Part I – results from the test flight on the space shuttle

Galactic secondary positron flux at the Earth

Antiproton Flux, Antiproton-to-Proton Flux Ratio, and Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station

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