A new measurement of the flux of the light cosmic-ray nuclei at high energies

Buckley, J. H.; Dwyer, J. R.; Mueller, D.; Swordy, S. P.; Tang, K. K.

doi:10.1086/174357

Cited by 58 publications

(38 citation statements)

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“…4.15 our data are only marginally in agreement with the spectrum used to calculate atmospheric neutrino spectra [31]. Our results are compared to recent balloon experiment results [23,28,53,54] in Fig. 4.16.…”

Section: Primary Spectrumsupporting

confidence: 81%

“…4.16. The primary helium ux spectrum multiplied by E 2:5 K in units of m −2 s −1 sr −1 (GeV=A) 1:5 in comparison with recent measurements: CAPRICE [23], RICH [28], BESS [53], IMAX [54].…”

Section: Second Spectrummentioning

confidence: 97%

“…Since no di erence in the rigidity spectra of protons and helium has been detected the same sources and propagation histories were inferred for both species [27]. However recent and more accurate measurements [21,28] suggest protons and helium may have di erent spectral indices in the range 10 -100 GeV. The most accurate experiments to date were balloon based [21][22][23], however even ∼5g=cm 2 of residual atmosphere was an important source of systematic errors.…”

Section: Introductionmentioning

confidence: 96%

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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

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Section: Primary Spectrumsupporting

confidence: 81%

Section: Second Spectrummentioning

confidence: 97%

Section: Introductionmentioning

confidence: 96%

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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

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“…Figure 1 shows a comparison between the BESS+JACEE fit, the data from [19,20], the fit from [21] (shaded areas) and several other experiments [22][23][24][25][26][27][28][29][30][31][32], performed in different periods of solar activity. The filled/shaded areas in fig.…”

Section: Primary Cosmic Ray Spectrum and Compositionmentioning

confidence: 99%

Atmospheric neutrino flux supported by recent muon experiments

2001

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We present a new one-dimensional calculation of low and intermediate energy atmospheric muon and neutrino fluxes, using up-to-date data on primary cosmic rays and hadronic interactions. We study several sources of uncertainties relevant to our calculations. A comparison with the muon fluxes and charge ratios measured in several modern balloon-borne experiments suggests that the atmospheric neutrino flux is essentially lower than one used for the standard analyses of the sub-GeV and multi-GeV neutrino induced events in underground detectors.

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“…A precise knowledge of such spectra is of particular importance to interpret the observational data from muon and neutrino detectors deep underground [12]. The measurement of the primary proton spectrum has been performed by means of satellite and balloon borne experiments [13][14][15][16][17][18][19][20][21][22][23][24][25][26] and indirectly derived by using ground based detectors [27][28][29][30]. In the region of tens of TeV, however, direct measurements lack statistics and moreover their energy determinations are not calorimetric and depend on the interaction parameters and their fluctuations.…”

Section: Introductionmentioning

confidence: 99%