Prompt neutrino fluxes from atmospheric charm

Enberg, Rikard; Reno, Mary Hall; Sarčević, Ina

doi:10.1103/physrevd.78.043005

Cited by 382 publications

(650 citation statements)

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“…Distribution of primary neutrino energies and zenith angles for conventional atmospheric [14,15], prompt atmospheric [13] and astrophysical ν μ þν μ expected in the runtime of 348.1 days, folded with the detection efficiency of this analysis. Note, the flux normalization of the latter two are multiplied by factors of 200 and 500 for better visibility in the right figure.…”

Section: Fig 1 (Color Online)mentioning

confidence: 99%

“…The cross sections for their production are small and therefore their contribution is only relevant at higher energies, where the conventional component is suppressed below this level [11][12][13]. These heavy mesons have such short lifetimes that they immediately decay, rather than interact, which causes prompt neutrinos to follow the energy spectrum of the parent cosmic rays.…”

Section: Introductionmentioning

confidence: 99%

“…The effect of the knee is implemented by folding the yield of neutrinos per primary nucleon with the primary spectrum of nucleons, as described in the Appendix. The prompt atmospheric neutrino flux is estimated according to the prediction by Enberg et al (ERS08) [13] as a baseline model, which has also been modified at high energies to take into account the cosmic-ray flux parametrizations of H3a and poly-gonato (see the Appendix).…”

Section: Fig 1 (Color Online)mentioning

confidence: 99%

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Search for a diffuse flux of astrophysical muon neutrinos with the IceCube 59-string configuration

Aartsen¹,

Abbasi²,

Ackermann³

et al. 2014

Phys. Rev. D

102

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when the array was running in its 59-string configuration. The data sample was optimized to contain muon neutrino induced events with a background contamination of atmospheric muons of less than 1%. These data, which are dominated by atmospheric neutrinos, are analyzed with a global likelihood fit to search for possible contributions of prompt atmospheric and astrophysical neutrinos, neither of which have yet been identified. Such signals are expected to follow a harder energy spectrum than conventional atmospheric neutrinos. In addition, the zenith angle distribution differs for astrophysical and atmospheric signals. A global fit of the reconstructed energies and directions of observed events is performed, including possible neutrino flux contributions for an astrophysical signal and atmospheric backgrounds as well as systematic uncertainties of the experiment and theoretical predictions. The best fit yields an astrophysical signal flux for ν μ þν μ of E 2 · ΦðEÞ ¼ 0.25 × 10 −8 GeV cm −2 s −1 sr −1 ,

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Section: Fig 1 (Color Online)mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Fig 1 (Color Online)mentioning

confidence: 99%

See 1 more Smart Citation

Search for a diffuse flux of astrophysical muon neutrinos with the IceCube 59-string configuration

Aartsen¹,

Abbasi²,

Ackermann³

et al. 2014

Phys. Rev. D

102

View full text Add to dashboard Cite

show abstract

“…The results of [27] and [28] are quite similar; we compare our curves for E p = 10 9 GeV and E p = 3.5 × 10 4 GeV (for BHPS model) with the corresponding curves of [27] (see figure 4). For this comparison we multiply our curves for dN/dx F on 2 · πR 2 A ≈ 600 mb.…”

Section: Resultsmentioning

confidence: 55%

“…Authors of [27,28] calculated the cross sections of inclusive cc-pair production using the colour dipole-model approach [29,30,31] (and extrinsic charm). The results of [27] and [28] are quite similar; we compare our curves for E p = 10 9 GeV and E p = 3.5 × 10 4 GeV (for BHPS model) with the corresponding curves of [27] (see figure 4).…”

Section: Resultsmentioning

confidence: 99%

About possible contribution of intrinsic charm component to inclusive spectra of charmed mesons

Bugaev¹,

Klimai²

2010

J. Phys. G: Nucl. Part. Phys.

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Abstract. We calculate differential energy spectra (x F -distributions) of charmed particles produced in proton-nucleus collisions, assuming the existence of intrinsic heavy quark components in the proton wave function. For the calculation, the recently proposed factorization scheme is used, based on the Color Glass Condensate theory and specially suited for predictions of a production of particles with large rapidities. It is argued that the intrinsic charm component can, if it exists, dominate in a sum of two components, intrinsic + extrinsic, of the inclusive spectrum of charmed particles produced in proton-nucleus collisions at high energies, in the region of medium x F , 0.15 < x F < 0.7, and can give noticeable contribution to atmospheric fluxes of prompt muons and neutrinos.

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The highest energy neutrinos: First evidence for cosmic origin

Halzen¹

2014

Astron Nachr

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Developments in neutrino astronomy have been to a great extent motivated by the search for the sources of the cosmic rays, leading at a very early stage to the concept of a cubic kilometer neutrino detector. Almost four decades later such an instrument, IceCube, is taking data and has produced the first evidence for a flux of high-energy neutrinos of cosmic origin. After a brief review of the history of the field, we will introduce IceCube and describe the first analysis of data taken with the completed instrument. The atmospheric neutrino flux cannot accommodate an excess of 28 neutrinos observed with energies above 60 TeV. We will briefly speculate on the origin of these events. Readers interested specifically in IceCube results may refer directly to Sect. 3.

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Prompt neutrino fluxes from atmospheric charm

Cited by 382 publications

References 100 publications

Search for a diffuse flux of astrophysical muon neutrinos with the IceCube 59-string configuration

Search for a diffuse flux of astrophysical muon neutrinos with the IceCube 59-string configuration

About possible contribution of intrinsic charm component to inclusive spectra of charmed mesons

The highest energy neutrinos: First evidence for cosmic origin

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