Measurements of 0.2–20GeV/n cosmic-ray proton and helium spectra from 1997 through 2002 with the BESS spectrometer

Shikaze, Y.; Haino, S.; Abe, K.; Fuke, H.; Hams, T.; Kim, K. C.; Makida, Y.; Matsuda, Shinya; Mitchell, J. W.; Моисеев, А. А.; Nishimura, Jun; Nozaki, M.; Orito, S.; Ormes, J. F.; Sanuki, T.; Sasaki, M.; Seo, E. S.; Streitmatter, R. E.; Suzuki, Jun–ichi; Tanaka, Kenichi; Yamagami, T.; Yamamoto, A.; Yoshida, Tetsuya; Yoshimura, K.

doi:10.1016/j.astropartphys.2007.05.001

Cited by 195 publications

(203 citation statements)

References 28 publications

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“…The solid lines refer to Kamae et al (2006), the dashed lines to , and the dotted lines to Tan & Ng (1983). For each set of curves, the thick lines are obtained for the proton spectrum parameterization of Donato et al (2001), while the thin lines refer to Shikaze et al (2007). Figure 2 illustrates that different parameterizations of the incident proton flux cause less significant uncertainty than the nuclear models.…”

Section: Incident Proton Fluxmentioning

confidence: 99%

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Galactic secondary positron flux at the Earth

Delahaye

Lineros²,

Donato³

et al. 2009

A&A

216

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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Section: Incident Proton Fluxmentioning

confidence: 99%

“…Various parameterizations of these measurements are found in the literature. In this analysis, we adopt the determinations of Shikaze et al (2007) and Donato et al (2001). The effect induced on the positron source term in Eq.…”

Section: Incident Proton Fluxmentioning

confidence: 99%

Galactic secondary positron flux at the Earth

Delahaye

Lineros²,

Donato³

et al. 2009

A&A

216

308

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“…This so-called solar modulation effect is more important for low energy CRs (see e.g., [60]) and its modeling is currently an active area of CR research. In this work, the inter-stellar spectra of all species are solar modulated according to a spherical force field approximation [61] with potential φ = 500GV, though in all cases we fit only to data in the range E > 10 GeV to minimize the importance of uncertainties in modeling this effect.…”

Section: Jhep01(2011)064mentioning

confidence: 99%

“…We thus begin by finding the values of the nucleon source parameters that best fit this data. We use the GALPROP default spatial distribution for nucleon sources and tune the overall JHEP01(2011)064 normalization and spectral index (i.e., the exponent of the power-law describing the energydependence of the sources) of these sources to best fit measurements of the proton absolute spectrum from BESS/BESS-TeV [60,64], AMS-01 [65], CAPRICE98 [66] and ATIC [67]. It is clear that the data favor a (locally-measured) spectral index of ≈ 2.75 ± 0.05, though the ATIC points stiffen somewhat above ∼ 1 TeV; including all four data sets, we find a best fit spectral index of γ n = 2.73 and normalization 3.96 × 10 −6 GeV −1 cm −2 sr −1 s −1 @ 100 GeV.…”

Section: Nucleon Source and Turbulent Diffusion Parametersmentioning

confidence: 99%

Cosmic ray anomalies from the MSSM?

Cotta

Conley

Gainer

et al. 2011

J. High Energ. Phys.

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Abstract:The recent positron excess in cosmic rays (CR) observed by the PAMELA satellite may be a signal for dark matter (DM) annihilation. When these measurements are combined with those from FERMI on the total (e + + e − ) flux and from PAMELA itself on thep/p ratio, these and other results are difficult to reconcile with traditional models of DM, including the conventional mSUGRA version of Supersymmetry even if boosts as large as 10 3−4 are allowed. In this paper, we combine the results of a previously obtained scan over a more general 19-parameter subspace of the MSSM with a corresponding scan over astrophysical parameters that describe the propagation of CR. We then ascertain whether or not a good fit to this CR data can be obtained with relatively small boost factors while simultaneously satisfying the additional constraints arising from gamma ray data. We find that a specific subclass of MSSM models where the LSP is mostly pure bino and annihilates almost exclusively into τ pairs comes very close to satisfying these requirements. The lightestτ in this set of models is found to be relatively close in mass to the LSP and is in some cases the nLSP. These models lead to a significant improvement in the overall fit to the data by an amount ∆χ 2 ∼ 1/dof in comparison to the best fit without Supersymmetry while employing boosts ∼ 100. The implications of these models for future experiments are discussed.

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“…4, we show the predicted HERD spectra for protons, helium nuclei, carbon nuclei and iron nuclei, in comparison with all previous direct measurements in space. Clearly HERD will surpass all previous results of directly measured cosmic rays from, e.g., AMS02 [13], ATIC-2 [14], BESS [15], CREAM, [16,17] HEAO [18], JACEE [19], PAMELA [20], RUNJOB [21], SOKOL [22] and TRACER [23], with much better statistics and up to much higher energies even beyond PeV and into the "knee" region. For example, at least ten events will be recorded from 900 TeV to 2 PeV for each specie, which means that the expected energy spectra of most nuclei will be directly extended to the knee range with much smaller error bars than previous direct measurements in space.…”

Section: Item Value Detectormentioning

confidence: 76%

Introduction to the High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Future Space Station

Zhang¹,

Adriani²,

Albergo³

et al. 2017

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

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PoS(ICRC2017)1077The High Energy cosmic-Radiation Detection (HERD) facility is one of several space astronomy payloads onboard China's Space Station, which is planned for operation starting around 2025 for about 10 years. The main scientific objectives of HERD are searching for signals of dark matter annihilation products, precise cosmic electron (plus positron) spectrum and anisotropy measurements up to 10 TeV, precise cosmic ray spectrum and composition measurements up to the knee energy, and high energy gamma-ray monitoring and survey. HERD is composed of a 3-D cubic calorimeter (CALO) surrounded by microstrip silicon trackers (STKs) from five sides except the bottom. CALO is made of about 7,500 cubes of LYSO crystals, corresponding to about 55 radiation lengths and 3 nuclear interaction lengths, respectively. The top STK microstrips of six X-Y layers are sandwiched with tungsten converters to make precise directional measurements of incoming electrons and gamma-rays. In the baseline design, each of the four side STKs is made of only three layers microstrips. All STKs will also be used for measuring the charge and incoming directions of cosmic rays, as well as identifying back scattered tracks. With this design, HERD can achieve the following performance: energy resolution of 1% for electrons and gamma-rays beyond 100 GeV and 20% for protons from 100 GeV to 1 PeV; electron/proton separation power better than 10 −5 ; effective geometrical factors of >3 m 2 sr for electron and diffuse gamma-rays, >2 m 2 sr for cosmic ray nuclei. R&D is under way for reading out the LYSO signals with optical fiber coupled to image intensified IsCMOS and CALO prototype of 250 LYSO crystals.

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Measurements of 0.2–20GeV/n cosmic-ray proton and helium spectra from 1997 through 2002 with the BESS spectrometer

Cited by 195 publications

References 28 publications

Galactic secondary positron flux at the Earth

Galactic secondary positron flux at the Earth

Cosmic ray anomalies from the MSSM?

Introduction to the High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Future Space Station

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