Measurement of Boron and Carbon Fluxes in Cosmic Rays With the Pamela Experiment

Adriani, O.; Barbarino, G. C.; Bazilevskaya, G. A.; Bellotti, R.; Boezio, M.; Bogomolov, É. A.; Bongi, M.; Bonvicini, V.; Bottai, S.; Bruno, A.; Cafagna, F.; Campana, D.; Carbone, R.; Carlson, P.; Casolino, M.; Castellini, G.; Danilchenko, I. A.; Donato, C. De; Santis, C. De; Simone, N. De; Felice, V. Di; Formato, V.; Galper, A. M.; Karelin, A. V.; Koldashov, S. V.; Koldobskiy, S.; Krutkov, S. Y.; Kvashnin, A. N.; Leonov, A.; Malakhov, V.; Marcelli, L.; Martucci, M.; Mayorov, A. G.; Menn, W.; Мерге, М.; Mikhailov, V. V.; Mocchiutti, E.; Monaco, A.; Mori, N.; Munini, R.; Osteria, G.; Palma, F.; Panico, B.; Papini, P.; Pearce, Mark; Picozza, P.; Pizzolotto, C.; Ricci, M.; Ricciarini, S.; Rossetto, L.; Sarkar, R.; Scotti, V.; Simon, M.; Sparvoli, R.; Спиллантини, П.; Stozhkov, Y. I.; Vacchi, A.; Vannuccini, E.; Vasilyev, G.; Voronov, S. A.; Yurkin, Y. T.; Zampa, G.; Zampa, N.; Zverev, V. G.

doi:10.1088/0004-637x/791/2/93

Cited by 174 publications

(167 citation statements)

References 38 publications

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“…The index δ of the rigidity dependence of the diffusion coefficient is derived from the slope of the secondaryto-primary ratio (e.g., B/C). A fit to the AMS-02 measurements of the B/C ratio [31] yields 0.395, which is very close to the value δ = 0.397 ± 0.007 found from the fit to the PAMELA data [34] and quite close to the Kolmogorov index of 1/3. The MCMC procedure prefers a medium size halo of 4 kpc, also favored in the past studies [35].…”

Section: Calculations and Resultssupporting

confidence: 81%

Inside out: unveiling local interstellar spectra of cosmic ray species

Boschini¹,

Torre²,

Gervasi³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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Local interstellar spectra (LIS) for protons, helium and antiprotons are built using the most recent experimental results combined with state-of-the-art models for propagation in the Galaxy and Heliosphere. Two propagation packages, GALPROP and HelMod, are combined to provide a single framework that is run to reproduce direct measurements of cosmic ray (CR) species at different modulation levels and at both polarities of the solar magnetic field. To do so in a selfconsistent way, an iterative procedure was developed, where the GALPROP LIS output is fed into HelMod that provides modulated spectra for specific time periods of selected experiments to compare with the data. The parameters were tuned with a maximum likelihood procedure using an extensive data set of proton spectra from 1997-2015. The proposed LIS accommodate both the low energy interstellar CR spectra measured by Voyager 1 and the high energy observations by BESS, PAMELA, AMS-01, and AMS-02 made from the balloons and near-Earth payloads. The proton LIS also accounts for Ulysses counting rate features measured out of the ecliptic plane. The obtained solution is in a good agreement with proton, helium, and antiproton data by AMS-02, BESS, and PAMELA in the whole energy range.

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Section: Calculations and Resultssupporting

confidence: 81%

Inside out: unveiling local interstellar spectra of cosmic ray species

Boschini¹,

Torre²,

Gervasi³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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show abstract

“…Another important milestone is an accurate measurement of the B/C ratio up to 100 GeV/nucleon by PAMELA [11] that is consistent with preliminary AMS-02 1 measurements reaching ∼400 GeV/nucleon. Both measurements indicate the index of the diffusion coefficient α ≈ 0.4 or even smaller [11] that supports a Kolmogorov-type power spectrum of interstellar turbulence [12], thus favoring the stochastic reacceleration model for interstellar propagation. Besides providing more accurate data over a wider energy range these new measurements give an important insight into CR acceleration and propagation processes.…”

Section: Introductionsupporting

confidence: 68%

New Calculation of Secondary Antiprotons in Cosmic Rays

Moskalenko¹

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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A dramatic increase in the accuracy and statistics of space-borne cosmic ray (CR) measurements has yielded several breakthroughs over the last several years. The most puzzling is the rise in the positron fraction above 10 GeV over the predictions of the propagation models assuming pure secondary production. Antiprotons are produced in CR interactions with interstellar gas and are, therefore, called secondary. These are the same interactions that produce charged and neutral mesons which decay to secondary electrons and positrons and γ-rays. However, in contrast to CR electrons and positrons that can be produced copiously in pulsars, there is no known astrophysical source of primaryp. Therefore,p data and their correct interpretation hold the key to the resolution of many astrophysical puzzles. We calculatedp production in pp-, pA-, and AA-interactions using EPOS-LHC and QGSJET-II-04, two of the most advanced Monte Carlo generators tuned to accelerator data including those from the LHC. The new cross sections are being incorporated into the GALPROP code to allow an accurate calculation of the spectrum of secondaryp in CRs.

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“…SNRs for SNe type II. To ensure that the propagation parameters are correct, we need to compare the model prediction with the boron-to-carbon ratio [5,[64][65][66] and the proton flux [62]. As shown in Fig.…”

Section: Propagation Parameters and E ± Backgroundmentioning

confidence: 99%

Pulsar interpretation of lepton spectra measured by AMS-02

Feng

Zhang

2016

Eur. Phys. J. C

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Alpha Magnetic Spectrometer (AMS-02) recently published its lepton spectra measurement. The results show that the positron fraction no longer increases above ∼200 GeV. The aim of this work is to investigate the possibility that the excess of positron fraction is due to pulsars. Nearby known pulsars from the ATNF catalog are considered to be a possible primary positron source of the high energy positrons. We find that the pulsars with age T (0.45−4.5) × 10 5 year and distance d < 0.5 kpc can explain the behavior of positron fraction of AMS-02 in the range of high energy. We show that each of the four pulsars-Geminga, J1741-2054, Monogem, and J0942-5552-is able to be a single source satisfying all considered physical requirements. We also discuss the possibility that these high energy e ± are from multiple pulsars. The multiple pulsar contribution predicts a positron fraction with some structures at higher energies.

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Measurement of Boron and Carbon Fluxes in Cosmic Rays With the Pamela Experiment

Cited by 174 publications

References 38 publications

Inside out: unveiling local interstellar spectra of cosmic ray species

Inside out: unveiling local interstellar spectra of cosmic ray species

New Calculation of Secondary Antiprotons in Cosmic Rays

Pulsar interpretation of lepton spectra measured by AMS-02

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