An extended Heitler–Matthews model for the full hadronic cascade in cosmic air showers

Montanus, J. M. C.

doi:10.1016/j.astropartphys.2014.03.010

Cited by 15 publications

(23 citation statements)

References 17 publications

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“…For the description of the hadronic component we adopt the extended Heitler-Matthews model, see Ref. [4]. A basic idea of the extended Heitler-Matthews model is visualized in Fig.1.…”

Section: Methodsmentioning

confidence: 99%

“…Charged pions further interact in the atmosphere and create other pions. A multiplicity M π of produced pions in the pion initiated interaction in the shower is energy dependent [4] M π ≈ 0.15 · E 0.18 .…”

Section: Methodsmentioning

confidence: 99%

“…Other necessary parameters of the model are the interaction lengths. For pions, protons and iron nuclei we adopt [4]…”

Section: Methodsmentioning

confidence: 99%

“…The Heitler-Matthews model is further modified to the extended Heitler-Matthews model presented in Ref. [4]. The extended Heitler-Matthews model includes the better description of pion interaction lengths and branching multiplicities.…”

Section: Introductionmentioning

confidence: 99%

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A branching model for hadronic air showers

Novotný¹,

Nosek²,

Ebr³

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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We introduce a simple branching model for the development of hadronic showers in the Earth's atmosphere. Based on this model, we show how the size of the pionic component followed by muons can be estimated. Several aspects of the subsequent muonic component are also discussed. We focus on the energy evolution of the muon production depth. We also estimate the impact of the primary particle mass on the size of the hadronic component. Even though a precise calculation of the development of air showers must be left to complex Monte Carlo simulations, the proposed model can reveal qualitative insight into the air shower physics.

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“…For the description of the hadronic component we adopt the extended Heitler-Matthews model, see Ref. [4]. A basic idea of the extended Heitler-Matthews model is visualized in Fig.1.…”

Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

“…Other necessary parameters of the model are the interaction lengths. For pions, protons and iron nuclei we adopt [4]…”

Section: Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

A branching model for hadronic air showers

Novotný¹,

Nosek²,

Ebr³

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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“…The description of of hadronic cascades relies on empirical hadronic interaction models. The Heitler model can be adapted to hadronic showers by assuming that after each interaction length λ I , N hadrons are produced, at each step with a certain fraction of energy divertedvia π 0 production -into electromagnetic showers [29,30]. The compared to λ r larger interaction length λ I is partly compensated by the larger multiplicity per interaction N , speeding up shower evolution.…”

Section: General Properties Of Showersmentioning

confidence: 99%

Detectors for high-energy messengers from the Universe

Hofmann

Hinton

2018

Nuclear Instruments and Methods in Physics Research Section A:

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High-energy messengers from the Universe comprise charged cosmic rays, gamma rays and neutrinos. Here we summarize the detection principles and detection schemes for these particles, with a focus on ground-based instruments which employ natural media such as air, ice, or water as their detection medium.High energy astrophysics is concerned with the study of non-thermal particle populations in our Galaxy and beyond, with their sources, propagation, and impact on their cosmic environment. This field relies on detectors for highenergy messengers from the Universe -the subject of this article -but also on astrophysical instruments in many other domains of the electromagnetic spectrum, most notably in the radio and X-ray, tracing the synchrotron radiation of high energy electrons. For the current discussion, we will -somewhat arbitrarily -concentrate on the domain from GeV energies up, where the detectors address common science themes and share many detection features; MeV instruments differ in terms of their science focus but also in their detection principles.2 Given that typical Galactic radiation fields provide U ≈ 1 eV/cm 3 , the lifetime of cosmic-ray electrons is limited to τyr ≈ 3 · 10 5 /E e,TeV and hence their range to √ Dτ ≈ 1kpc/E 0.25 e,TeV .

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