Some problems and perspectives in cosmic-ray studies

Grigorov, N. L.; Rapoport, Iris; Savenko, I. A.; Skuridin, G. A.

doi:10.1007/bf00241054

Cited by 6 publications

(6 citation statements)

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“…CREAM also has excellent charge resolution, sufficient to clearly identify individual nuclei, whereas JACEE and RUNJOB reported elemental groups. Our observation did not confirm a softer spectrum of protons above 2 TeV reported by Grigorov et al (1970) or a bend around 40 TeV (Asakimori et al 1993a). An increase in the flux of helium relative to protons could be interpreted as evidence for two different types of sources for protons and helium nuclei as proposed by Biermann (1993).…”

Section: Discussioncontrasting

confidence: 94%

Cosmic-Ray Proton and Helium Spectra From the First Cream Flight

Yoon

Ahn

Allison

et al. 2011

ApJ

349

253

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Cosmic-ray proton and helium spectra have been measured with the balloon-borne Cosmic Ray Energetics And Mass experiment flown for 42 days in Antarctica in the 2004-2005 austral summer season. High-energy cosmic-ray data were collected at an average altitude of ∼38.5 km with an average atmospheric overburden of ∼3.9 g cm −2 . Individual elements are clearly separated with a charge resolution of ∼0.15 e (in charge units) and ∼0.2 e for protons and helium nuclei, respectively. The measured spectra at the top of the atmosphere are represented by power laws with a spectral index of −2.66 ± 0.02 for protons from 2.5 TeV to 250 TeV and -2.58 ± 0.02 for helium nuclei from 630 GeV nucleon −1 to 63 TeV nucleon −1 . They are harder than previous measurements

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Section: Discussioncontrasting

confidence: 94%

Cosmic-Ray Proton and Helium Spectra From the First Cream Flight

Yoon

Ahn

Allison

et al. 2011

ApJ

349

253

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“…[77]) we notice that it is mainly driven by the cosmic-ray data reported in Ref. [63] (open circles in Fig. 1) which are subject to 043017-4 FIG.…”

Section: E Global Fitmentioning

confidence: 69%

Dark matter or correlated errors: Systematics of the AMS-02 antiproton excess

Heisig

Korsmeier

Winkler

2020

Phys. Rev. Research

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Several studies have pointed out an excess in the AMS-02 antiproton spectrum at rigidities of 10-20 GV. Its spectral properties were found to be consistent with a dark-matter particle of mass 50-100 GeV which annihilates hadronically at roughly the thermal rate. In this paper, we reinvestigate the antiproton excess, including all relevant sources of systematic errors. Most importantly, we perform a realistic estimate of the correlations in the AMS-02 systematic error which could potentially "fake" a dark-matter signal. The dominant systematics in the relevant rigidity range originate from uncertainties in the cross sections for absorption of cosmic rays within the detector material. We calculate their correlations within the Glauber-Gribov theory of inelastic scattering. The AMS-02 correlations enter our spectral search for dark matter in the form of covariance matrices, which we make publicly available for the cosmic-ray community. We find that the global significance of the antiproton excess is reduced to below 1 σ once all systematics, including the derived AMS-02 error correlations, are taken into account. No significant preference for a dark-matter signal in the AMS-02 antiproton data is found in the mass range 10-10 000 GeV.

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“…The only direct measurements which have been performed in the same energy range are those from the Proton I and Proton II satellite experiments of Grigorov et al 6 We disagree with the results of Grigorov et a/. 6 by a factor of about 2.…”

Section: Discussionmentioning

confidence: 55%

“…6 by a factor of about 2. We feel that several arguments exist which seem to indicate that their spectrum may be erroneous.…”

Section: Discussionmentioning

confidence: 97%

Measurement of the Primary Cosmic-Ray Proton Spectrum between 40 and 400 GeV

et al. 1969

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It is a simple matter to verify that the second double sum involving d ftPiXlc does not contribute to the stressenergy tensor. The /=m=0 term of the first double sum is excluded, of course, by definition (2). The part of the first sum, with w=0, Z^O, gives the zero-temperature contribution to the stress-energy tensor which we have already considered; the part with 1=0, w^O gives the blackbody contribution which we have just discussed.It is straightforward to show that the sum remaining with neither / nor m vanishing gives the finite-temperature, finite-plate separation correction quoted in Eqs. (17)-(22). ACKNOWLEDGMENTSWe have enjoyed fruitful conversations on this topic with David Boulware and Robert Puff.Equipment consisting of an ionization spectrometer and spark chambers has been exposed to primary cosmic rays in a balloon flight which allowed a data collection time of 14.3 h at an altitude of 5.7 g/cm 2 . The purpose of this experiment was to study the flux, composition, possible time variations, and nuclear interaction properties of cosmic rays at energies between 44) and 400 GeV. The apparatus has also been exposed to 10-, 20.5-, and 28-GeV/c protons at the Brookhaven AGS in order to study the spectrometer response at three known energies and to be able to extrapolate this response to higher energies. The integral energy spectrum of primary cosmic-ray protons between 40 and 400 GeV was found to be n(>E 0 ) = (0.91.o.2 +0 -8 ) £o _1 -7±01 (E in GeV). The corresponding intensity is a factor of 2 lower than that obtained from the Proton I and II satellite experiments.

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Some problems and perspectives in cosmic-ray studies

Cited by 6 publications

References 0 publications

Cosmic-Ray Proton and Helium Spectra From the First Cream Flight

Cosmic-Ray Proton and Helium Spectra From the First Cream Flight

Dark matter or correlated errors: Systematics of the AMS-02 antiproton excess

Measurement of the Primary Cosmic-Ray Proton Spectrum between 40 and 400 GeV

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