Calculations on the arrival-time distribution and energy content of extensive air showers at large core distances

Baxter, A. J.

doi:10.1088/0305-4470/2/1/008

Cited by 23 publications

(4 citation statements)

References 9 publications

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“…50 g cm-2 lower in the atmosphere and having sizes a t sea level some 50 % smaller than cascades derived under approximation B. A similar conclusion is reached by Marsden (1971), who compares cascades derived under approximation B with others derived from approximation A with the numerical data of Baxter (1969).…”

Section: Gen E R a L Sh O W Er Da Ta (A)supporting

confidence: 68%

Computer simulations of cosmic-ray air showers I. Average characteristics of proton initiated showers

Dixon

Earnshaw

Hook

et al. 1974

Proc. R. Soc. Lond. A

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Computer simulations have been made of the average characteristics of extensive air showers initiated by primary protons in a wide range of energy. The simulations, which are perhaps unusual in the detailed information available for each shower, have been made as part of a design study for future experiments intended to identify the mass number of energetic primaries. The sensitivity of the data from our simulations to the detail of the adopted model for interactions has been investigated by incorporating the consequences of the results from recent accelerator and cosmic ray experiments. The simulations have been made by means of a variety of computational techniques; in most simulations a simple representation of the interaction of high-energy nucleons and pions has been employed which is characterized by accounting well for presently available experimental data on large air showers. We conclude that the treatment of showers, although derived with a simple model for interactions, may be usefully employed to study the fluctuations in air-shower development.

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Section: Gen E R a L Sh O W Er Da Ta (A)supporting

confidence: 68%

Computer simulations of cosmic-ray air showers I. Average characteristics of proton initiated showers

Dixon

Earnshaw

Hook

et al. 1974

Proc. R. Soc. Lond. A

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“…Regarding the risetime of the signals, Linsley and Scarsi [32] demonstrated that the thickness of the disc of particles in the shower increased from a few meters near the axis to several hundreds of meters at large distances. Using Haverah Park data, a study showed that the spread of the arrival time distribution was decreased by attenuation across the array [33].…”

Section: Concept Of Azimuthal Asymmetry In the Risetimementioning

confidence: 99%

“…R. Vasquez, 36 J.R. Vázquez, 17 R.A. Vázquez, 13 D. Veberič, 33 V. Verzi, 47 J. Vicha, 30 M. Videla, 10 L. Villaseñor, 49 S. Vorobiov, 73 H. Wahlberg, 70 O. Wainberg, 10,11 D. Walz, 40 A.A. Watson, 99 M. Weber, 76 A. Weindl, 33 L. Wiencke, 81 H. Wilczyński, 37 T. Winchen, 25 D. Wittkowski, 25 B. Wundheiler, 10 S. Wykes, 42 L. Yang, 73 T. Yapici, 51 D. Yelos, 11,10 A. Yushkov, 1 E. Zas, 13 D. Zavrtanik, 73, 72 M. Zavrtanik, 72, 73 A. Zepeda, 85 B. Zimmermann, 76 M. Ziolkowski, 1 Z. Zong, 64 and F. Zuccarello 43,44 (The Pierre Auger Collaboration) *…”

mentioning

confidence: 99%

Azimuthal asymmetry in the risetime of the surface detector signals of the Pierre Auger Observatory

Aab¹,

Abreu²,

Aglietta³

et al. 2016

Phys. Rev. D

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The azimuthal asymmetry in the risetime of signals in Auger surface detector stations is a source of information on shower development. The azimuthal asymmetry is due to a combination of the longitudinal evolution of the shower and geometrical effects related to the angles of incidence of the particles into the detectors. The magnitude of the effect depends upon the zenith angle and state of development of the shower and thus provides a novel observable, (sec θ)max, sensitive to the 4 mass composition of cosmic rays above 3 × 10 18 eV. By comparing measurements with predictions from shower simulations, we find for both of our adopted models of hadronic physics (QGSJETII-04 and EPOS-LHC) an indication that the mean cosmic-ray mass increases slowly with energy, as has been inferred from other studies. However, the mass estimates are dependent on the shower model and on the range of distance from the shower core selected. Thus the method has uncovered further deficiencies in our understanding of shower modelling that must be resolved before the mass composition can be inferred from (sec θ)max.

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“…At 500 m from the axis of an event produced by a primary particle of ∼ 10 18 eV about half of the energy flow is carried by electrons and photons that are very largely absorbed in the water with the remaining energy being carried by muons. It was found the E 100 was ∼ 1/160th of the primary energy [Baxter, 1969]. This method of estimating the primary energy was used to argue that a shower of energy > 5 · 10 19 eV had been detected at Haverah Park soon after the Greisen-Zatsepin-Kuzmin prediction (1966) that such events should be rare [Andrews, 1968].…”

Section: Haverah Parkmentioning

confidence: 99%

Extensive air showers and ultra high-energy cosmic rays: a historical review

Kampert

Watson

2012

EPJ H

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Abstract. The discovery of extensive air showers by Rossi, Schmeiser, Bothe, Kolhörster and Auger at the end of the 1930s, facilitated by the coincidence technique of Bothe and Rossi, led to fundamental contributions in the field of cosmic ray physics and laid the foundation for high-energy particle physics. Soon after World War II a cosmic ray group at MIT in the USA pioneered detailed investigations of air shower phenomena and their experimental skill laid the foundation for many of the methods and much of the instrumentation used today. Soon interests focussed on the highest energies requiring much larger detectors to be operated. The first detection of air fluorescence light by Japanese and US groups in the early 1970s marked an important experimental breakthrough towards this end as it allowed huge volumes of atmosphere to be monitored by optical telescopes. Radio observations of air showers, pioneered in the 1960s, are presently experiencing a renaissance and may revolutionise the field again. In the last 7 decades the research has seen many ups but also a few downs. However, the example of the Cygnus X-3 story demonstrated that even non-confirmable observations can have a huge impact by boosting new instrumentation to make discoveries and shape an entire scientific community.

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Calculations on the arrival-time distribution and energy content of extensive air showers at large core distances

Cited by 23 publications

References 9 publications

Computer simulations of cosmic-ray air showers I. Average characteristics of proton initiated showers

Computer simulations of cosmic-ray air showers I. Average characteristics of proton initiated showers

Azimuthal asymmetry in the risetime of the surface detector signals of the Pierre Auger Observatory

Extensive air showers and ultra high-energy cosmic rays: a historical review

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