Current issues in open charm hadroproduction and new preliminary results from Fermilab E769

Karchin, P. E.

doi:10.2172/119984

Cited by 2 publications

(1 citation statement)

References 13 publications

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“…Since the process is basically a soft non-perturbative process it may be reasonable to assume that its energy dependence is the same as that for normal inelastic scattering [61,68]. We therefore take as our first case IC1 : σ IC (s) = 3 · 10 −5 σ inel (s) (44) with normalisation from [63] and shown as curve IC1 in Fig. 7.…”

Section: Possible Non-perturbative Origin Of Charmmentioning

confidence: 99%

Charm production and high energy atmospheric muon and neutrino fluxes

Thunman

Ingelman

Gondolo

1996

Astroparticle Physics

183

202

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Production of muons and neutrinos in cosmic ray interactions with the atmosphere has been investigated with Monte Carlo models for hadronic interactions. The resulting conventional muon and neutrino fluxes (from π and K decays) agree well with earlier calculations, whereas our prompt fluxes from charm decays are significantly lower than earlier estimates. Charm production is mainly considered as a well defined perturbative QCD process, but we also investigate a hypothetical nonperturbative intrinsic charm component in the proton. The lower charm rate implies better prospects for detecting very high energy neutrinos from cosmic sources. IntroductionThe flux of muons and neutrinos at the earth has an important contribution from decays of particles produced through the interaction of cosmic rays in the atmosphere (for a recent introduction see [1]). This has an interest in its own right, since it reflects primary interactions at energies that can by far exceed the highest available accelerator energies. It is also a background in studies of neutrinos from cosmic sources as attempted in large neutrino telescopes, such as Amanda [2], Baikal [3], Dumand [4] and Nestor [5].Here we present a detailed study of muon and neutrino production in cosmic ray interactions with nuclei in the atmosphere using Monte Carlo simulations [6].At GeV energies the atmospheric muon and neutrino fluxes are dominated by 'conventional' sources, i.e. decays of relatively long-lived particles such as π and K mesons. This is well understood from earlier studies [7,8,9], with which our investigations agree. With increasing energy, the probability increases that such particles interact in the atmosphere before decaying. This implies that even a small fraction of short-lived particles can give the dominant contribution to high energy muon and neutrino fluxes. These 'prompt' muons and neutrinos arise through semi-leptonic decays of hadrons containing heavy quarks, most notably charm.Available data in the multi-TeV energy range, obtained with surface and underground detectors (see e.g. refs. [10][11][12][13]), are still too discrepant to draw definitive conclusions on the flux of 1 thunman@tsl.uu.se 2 ingelman@tsl.uu.se, also at DESY, Hamburg.

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Section: Possible Non-perturbative Origin Of Charmmentioning

confidence: 99%

Charm production and high energy atmospheric muon and neutrino fluxes

Thunman

Ingelman

Gondolo

1996

Astroparticle Physics

183

202

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Signals for intrinsic charm in high energy interactions

Ingelman

Thunman

1997

Zeitschrift f�r Physik C Particles and Fields

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The prospects to test the hypothesis of intrinsic charm quarks in the proton are investigated. We consider how this component can be directly or indirectly probed in deep inelastic scattering at HERA and in fixed target experiments and find that an overlooked signal might be present in existing NMC data. Applying the intrinsic charm model to hadron collisions we compare the resulting charm production cross-sections with those based on standard perturbative QCD and available data. Extrapolating to higher energies we obtain predictions for charm production at the Tevatron and LHC.

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Current issues in open charm hadroproduction and new preliminary results from Fermilab E769

Cited by 2 publications

References 13 publications

Charm production and high energy atmospheric muon and neutrino fluxes

Charm production and high energy atmospheric muon and neutrino fluxes

Signals for intrinsic charm in high energy interactions

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