CORSIKA implementation of heavy quark production and propagation in extensive air showers

Bueno, A.; Gascón, A.

doi:10.1016/j.cpc.2013.09.025

Cited by 8 publications

(14 citation statements)

References 57 publications

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“…We use the approach of Ref. [40] to parametrize their energy loss distribution. The observable effect of multiple charm interactions is the production of a lowenergy muon after a semileptonic decay, mimicking a high inelasticity track for ν e or ν τ interactions.…”

Section: B Neutrino Interactions and Cherenkov Light Emissionmentioning

confidence: 99%

Measurements using the inelasticity distribution of multi-TeV neutrino interactions in IceCube

Aartsen¹,

Anton²,

Ansseau³

et al. 2019

Phys. Rev. D

141

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Inelasticity, the fraction of a neutrino's energy transferred to hadrons, is a quantity of interest in the study of astrophysical and atmospheric neutrino interactions at multi-TeV energies with IceCube. In this work, a sample of contained neutrino interactions in IceCube is obtained from five years of data and classified as 2650 tracks and 965 cascades. Tracks arise predominantly from charged-current ν μ interactions, and we demonstrate that we can reconstruct their energy and inelasticity. The inelasticity distribution is found to be consistent with the calculation of Cooper-Sarkar et al. across the energy range from ∼1 to ∼100 TeV. Along with cascades from neutrinos of all flavors, we also perform a fit over the energy, zenith angle, and inelasticity distribution to characterize the flux of astrophysical and atmospheric neutrinos. The energy spectrum of diffuse astrophysical neutrinos is described well by a power law in both track and cascade samples, and a best-fit index γ ¼ 2.62 AE 0.07 is found in the energy range from 3.5 TeV to 2.6 PeV. Limits are set on the astrophysical flavor composition and are compatible with a ratio of ð 1 3 ∶ 1 3 ∶ 1 3 Þ ⊕. Exploiting the distinct inelasticity distribution of ν μ andν μ interactions, the atmospheric ν μ toν μ flux ratio in the energy range from 770 GeV to 21 TeV is found to be 0.77 þ0.44 −0.25 times the calculation by Honda et al. Lastly, the inelasticity distribution is also sensitive to neutrino charged-current charm production. The data are consistent with a leading-order calculation, with zero charm production excluded at 91% confidence level. Future analyses of inelasticity distributions may probe new physics that affects neutrino interactions both in and beyond the Standard Model.

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Section: B Neutrino Interactions and Cherenkov Light Emissionmentioning

confidence: 99%

Measurements using the inelasticity distribution of multi-TeV neutrino interactions in IceCube

Aartsen¹,

Anton²,

Ansseau³

et al. 2019

Phys. Rev. D

141

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“…The co-moving heavy and valence quarks have the same rapidity in these states but the larger mass of the heavy quarks implies they carries most of the projectile momentum. Heavy hadrons form from these states can have a large longitudinal momentum and carry a large fraction of the primary energy, which is crucial for their propagation [4]. At the figure 1 we can see the differential energy fraction distribution for some charmed and bottom hadrons.…”

Section: Intrinsic Quark Modelmentioning

confidence: 96%

“…QGSJET01). Through key SIGMAQ, the cross sections for the charm and bottom mesons and baryons are determined [4].…”

Section: Heavy Particle Simulationmentioning

confidence: 99%

Longitudinal profiles of Extensive Air Showers with inclusion of charm and bottom particles

Müller

Gonçalves

2019

Int. J. Mod. Phys. A

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Charm and bottom particles are rare in Extensive Air Showers but the effect of its presence can be radical in the development of the Extensive Air Showers (EAS). If such particles arise with a large fraction of the primary energy, they can reach large atmospheric depths, depositing its energy in deeper layers of the atmosphere. As a consequence, the EAS observables (X max , RM S and N max ) will be modified, as well as the shape of the longitudinal profile of the energy deposited in the atmosphere. In this paper, we will modify the CORSIKA Monte Carlo by the inclusion of charm and bottom production in the first interaction of the primary cosmic ray. Results for different selections of the typical x F values of the heavy particles and distinct production models will be presented.

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“…In this contribution we will estimate the prompt muon and neutrino fluxes considering a modified version of the CORSIKA (Cosmic Ray Simulations for Kaskade) Monte Carlo [6], hereafter denoted HQ CORSIKA, which includes the charm and bottom production at the cosmic ray first interaction (For more details see Refs. [7,8]. In order to estimate the impact of the heavy particles in the EAS development, we will compare our predictions with those derived using the standard version of the CORSIKA (STD CORSIKA).…”

Section: Introductionmentioning

confidence: 99%

Angular distribution of prompt neutrinos in Extensive Air Showers

Müller¹,

Gonçalves²

2019

Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019)

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CORSIKA implementation of heavy quark production and propagation in extensive air showers

Cited by 8 publications

References 57 publications

Measurements using the inelasticity distribution of multi-TeV neutrino interactions in IceCube

Measurements using the inelasticity distribution of multi-TeV neutrino interactions in IceCube

Longitudinal profiles of Extensive Air Showers with inclusion of charm and bottom particles

Angular distribution of prompt neutrinos in Extensive Air Showers

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