Production of antiprotons in the upper atmosphere by interacting primary cosmic rays

Pfeifer, C.; Roesler, S.; Simon, M.

doi:10.1103/physrevc.54.882

Cited by 21 publications

(5 citation statements)

References 31 publications

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“…The data were corrected for the losses of these events with multiplicative factors that took into account the di †erent materials in the detector using the expressions for the interaction mean free path given by Pfeifer, Roesler, & Simon (1996) and by Stephens (1997). The corrected number of protons, hydrogen, and helium nuclei at the top of the payload are given in Tables 1 and 2.…”

Section: Calorimeter Efficiencymentioning

confidence: 99%

The Cosmic‐Ray Proton and Helium Spectra between 0.4 and 200 GV

Boezio

Carlson

Francke

et al. 1999

ApJ

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193

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We report on the hydrogen nuclei (protons and deuterons) spectrum from 0.15 to 200 GeV and on the helium nuclei spectrum over the energy range from 0.2 to 100 GeV nucleon~1 at the top of the atmosphere measured by the balloon-borne experiment Cosmic Antiparticle Ring-Imaging Cerenkov Experiment (CAPRICE), which was Ñown from Lynn Lake, Manitoba, Canada, on 1994 August 8È9. We also report on the proton spectrum over the energy range from 0.15 to 4.2 GeV. The experiment used the NMSU-WiZard/CAPRICE balloon-borne magnet spectrometer equipped with a solid radiator RingImaging Cerenkov (RICH) detector and a silicon-tungsten calorimeter for particle identiÐcation. This was the Ðrst time a RICH was used together with an imaging calorimeter in a balloon-borne experiment. These detectors allowed for clear particle identiÐcation, as well as excellent control of the detector efficiencies. The data were collected during 18 hr at a residual mean atmospheric depth of 3.9 g cm~2. With this apparatus 516,463 hydrogen and 32,457 helium nuclei were identiÐed in the rigidity range 0.4 to 200 GV and 1.2 to 200 GV, respectively. The observed energy spectrum at the top of the atmosphere can be represented by (1.1^0

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Section: Calorimeter Efficiencymentioning

confidence: 99%

The Cosmic‐Ray Proton and Helium Spectra between 0.4 and 200 GV

Boezio

Carlson

Francke

et al. 1999

ApJ

Self Cite

193

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“…The calculated background of secondary antiprotons and protons produced in the atmosphere was based on Pfeifer et al [14] for the antiprotons and Papini et al [15] for the protons. Interaction and annihilation losses are based on the measured cross sections quoted in Kuzichev et al [16] and Denisov et al [17], accounting in detail for the total material traversed by a particle in passing through the atmosphere, aluminum shell, and detector material.…”

Section: Figmentioning

confidence: 99%

Measurement of the Cosmic-Ray Antiproton-to-Proton Abundance Ratio between 4 and 50 GeV

et al. 2001

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We present a new measurement of the antiproton to proton abundance ratio, p/p, in the cosmic radiation. The HEAT-pbar instrument, a balloon borne magnet spectrometer with precise rigidity and multiple energy loss measurement capability, was flown successfully in Spring 2000, at an average atmospheric depth of 7.2 g/cm 2 . A total of 71 antiprotons were identified above the vertical geomagnetic cut-off rigidity of 4.2 GV. The highest measured proton energy was 81 GeV. We find that the p/p abundance ratio agrees with that expected from a purely secondary origin of antiprotons produced by primary protons with a standard soft energy spectrum.

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“…If the physic used by FLUKA is very accurate, cosmic rays spectra is not. As noted in [25] the flux can vary by a factor 2 leading to the same error factor for atmospheric neutrons. For the solar proton events we assume an uniformly distributed spectra, but these events are very often anisotropic [26].…”

Section: Discussionmentioning

confidence: 91%