A Monte Carlo calculation of atmospheric muon and neutrino fluxes

Thunman, Mats; Ingelman, G.; Gondolo, Paolo

doi:10.1016/0920-5632(95)00489-v

Cited by 7 publications

(16 citation statements)

References 5 publications

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“…A topic not discussed in this paper is cosmic ray physics where the momentum spectra of charm and bottom hadrons has implications for the rate of prompt leptons and neutrinos in atmospheric cascades [46]. Also here our improved modelling may affect the traditional flux calculations.…”

Section: Discussionmentioning

confidence: 99%

Production and hadronization of heavy quarks

2000

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Heavy long-lived quarks, i.e. charm and bottom, are frequently studied both as tests of QCD and as probes for other physics aspects within and beyond the standard model. The long life-time implies that charm and bottom hadrons are formed and observed. This hadronization process cannot be studied in isolation, but depends on the production environment. Within the framework of the string model, a major effect is the drag from the other end of the string that the c/b quark belongs to. In extreme cases, a small-mass string can collapse to a single hadron, thereby giving a nonuniversal flavour composition to the produced hadrons. We here develop and present a detailed model for the charm/bottom hadronization process, involving the various aspects of string fragmentation and collapse, and put it in the context of several heavy-flavour production sources. Applications are presented from fixed-target to LHC energies.

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Section: Discussionmentioning

confidence: 99%

Production and hadronization of heavy quarks

2000

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“…Following TIG [11], we neglect the detailed cosmic ray composition and consider all primaries to be nucleons with energy spectrum…”

Section: The Primary Cosmic Ray Fluxmentioning

confidence: 99%

“…The primary flux is attenuated as it penetrates into the atmosphere by collisions against the air nuclei. An approximate expression for the intensity of the primary flux at a depth X is (see [11] again)…”

Section: The Primary Cosmic Ray Fluxmentioning

confidence: 99%

“…A study based on pQCD was therefore performed in Ref. [11] (called TIG from now on). CLEO and HERA results were incorporated, but for simplicity the LO charm production cross section was adopted, multiplied by a constant K factor of 2 to bring it in line with the next-to-leading order values, and supplemented by parton shower evolution and hadronization according to the Lund model.…”

Section: Introductionmentioning

confidence: 99%

“…(a) Total cross sections for charm production σ cc up to NLO, for different PDFs, compared to the one used in the TIG model[11] (for MRS R1 we also show the Born cross section). (b) Related K c factors.…”

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confidence: 99%

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Prompt atmospheric neutrinos and muons: NLO versus LO QCD predictions

2000

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We compare the leading and next-to-leading order QCD predictions for the flux of atmospheric muons and neutrinos from decays of charmed particles. We find that the full NLO lepton fluxes can be approximated to within ϳ10% by the Born-level fluxes multiplied by an overall factor of 2.2Ϫ2.4, which depends slightly on the PDF. This supports the approach of Thunman, Ingelman and Gondolo. We also find that their very low lepton fluxes are due to the mild slope they used for the gluon distribution function at small momentum fractions, and that substantially larger lepton fluxes result when the slope of the gluon distribution function at small momentum fractions is larger.

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Atmospheric muons and neutrinos from charm

Gondolo

Ingelman

Thunman

1996

Nuclear Physics B - Proceedings Supplements

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We have updated our previous investigation of the production of muons and neutrinos in cosmic ray interactions with the atmosphere, taking account of recent results from the $ep$ collider HERA in our QCD-based model for hadronic interactions. Qualitatively, our previous results remain unmodified: our predictions for the conventional muon and neutrino fluxes agree with earlier calculations, whereas the charm particle treatment we use gives significantly lower prompt fluxes compared to earlier estimates. This implies better prospects for detecting very high energy neutrinos from cosmic sources.Comment: Talk presented by P. Gondolo at TAUP95, Toledo, Sept. 1995. 3 pages, 2 Postscript figures, uses epsf.sty and espcrc2.st

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A Monte Carlo calculation of atmospheric muon and neutrino fluxes

Cited by 7 publications

References 5 publications

Production and hadronization of heavy quarks

Production and hadronization of heavy quarks

Prompt atmospheric neutrinos and muons: NLO versus LO QCD predictions

Atmospheric muons and neutrinos from charm

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