EAS hadronic component as registered by a neutron monitor

Balabin, Yu. V.; Gvozdevsky, B. B.; Vashenyuk, É. V.; Dzhappuev, D. D.

doi:10.5194/astra-7-507-2011

Cited by 8 publications

(3 citation statements)

References 4 publications

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“…According to the developers of the neutron monitor data recording system from the Polar Geophysical Institute, the outliers are of physical origin and are caused by the arrival of ultrahigh-energy particles that produce multiple stars in the body of the monitor. Special studies of this phenomenon are being pursued [Balabin et al, 2011;Balabin et al, 2015].…”

Section: Resultsmentioning

confidence: 99%

Shape of spectrum of galactic cosmic ray intensity fluctuations

Starodubtsev

2022

Solar-Terrestrial Physics

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The impact of solar wind plasma on fluxes of galactic cosmic rays (CR) penetrating from the outside into the heliosphere with energies above ~1 GeV leads to temporal variations in the CR intensity in a wide frequency range. Cosmic rays being charged particles, their modulation occurs mainly under impacts of the interplanetary magnetic field. It is well known that the observed spectrum of interplanetary magnetic field (IMF) fluctuations in a wide frequency range ν from ~10–7 to ~10 Hz has a pronounced falling character and consists of three sections: energy, inertial, and dissipative. Each of them is described by the power law PIMF(ν)~ν–α, while the IMF spectrum index α increases with increasing frequency. The IMF fluctuations in each of these sections are also characterized by properties that depend on their nature. Also known are established links between fluctuation spectra of the interplanetary magnetic field and galactic cosmic rays in the case of modulation of the latter by Alfvén or fast magnetosonic waves. The theory predicts that fluctuation spectra of cosmic rays should also be described by the power law PCR(ν)~ν–γ. However, the results of many years of SHICRA SB RAS research into the nature and properties of cosmic ray intensity fluctuations based on data from neutron monitors at stations with different geomagnetic cut-offs RC from 0.5 to 6.3 GV show that the observed spectrum of fluctuations in galactic cosmic ray intensity in the frequency range above 10–4 Hz becomes flat, i.e. it is similar to white noise. This fact needs to be realized and explained. This paper reports the results of research into the shape of the spectrum of galactic cosmic ray intensity fluctuations within a frequency range ν from ~10–6 to ~1 Hz and compares them with model calculations of white noise spectra, using measurement data from the neutron monitor of the Apatity station. A possible physical explanation has been given for the observed shape of the cosmic ray fluctuation spectrum on the basis of the known mechanisms of their modulation in the heliosphere.

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Section: Resultsmentioning

confidence: 99%

Shape of spectrum of galactic cosmic ray intensity fluctuations

Starodubtsev

2022

Solar-Terrestrial Physics

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“…Measurement of delayed low-energy hadrons after the arrival of a cosmic-ray Extended Air Shower (EAS) can be an effective probe to determine whether an EAS is hadronic in origin. Neutrons have been found to arrive up to a millisecond after the detection of the core electromagnetic component of an EAS [1]. Simulation studies have reported that the delay is largely dependent on the neutron energy, with a flux of much lower energy thermalised neutrons arriving many milliseconds after the initial EAS [2].…”

Section: Introductionmentioning

confidence: 99%

Gadolinium loaded Cherenkov detectors for neutron monitoring in high energy air showers

et al. 2022

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Monitoring of high energy cosmic ray neutrons is of particular interest for cosmic ray water Cherenkov detectors as intense bundles of delayed neutrons have been found to arrive after the initial passage of a high energy air shower. In this paper we explore the possibility of building large-area high-energy neutron monitors using gadolinium-loaded Water Cherenkov Detectors (WCDs). GEANT4 simulations of photon production in WCDs are used to estimate the maximum detection efficiency for a hypothetical system. Requiring a series of neutron induced gamma ray flashes distributed over an extended period of time (up to 20 μs) was shown to be an effective way to discriminate high energy neutron interactions from other backgrounds. Results suggest that neutron detection efficiencies of 4–15% may be possible using a gadolinium-loaded detection system above 200 MeV. The magnitude of gadolinium loading was also shown to significantly modify the timing response of the simulated detector.

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Section: Introductionmentioning

confidence: 99%

Gadolinium Loaded Cherenkov Detectors for Neutron Monitoring in High Energy Air Showers

Stowell,

Fargher,

Thompson

et al. 2021

Preprint

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Monitoring of high energy cosmic ray neutrons is of particular interest for cosmic ray water Cherenkov detectors as intense bundles of delayed neutrons have been found to arrive after the initial passage of a high energy air shower. In this paper we explore the possibility of building largearea high-energy neutron monitors using gadolinium-loaded Water Cherenkov Detectors (WCDs). GEANT4 simulations of photon production in WCDs are used to estimate the maximum detection efficiency for a hypothetical system. Requiring a series of neutron induced gamma ray flashes distributed over an extended period of time (up to 20𝜇s) was shown to be an effective way to discriminate high energy neutron interactions from other backgrounds. Results suggest that neutron detection efficiencies of 4-15% may be possible using a gadolinium-loaded detection system above 200 MeV. The magnitude of gadolinium loading was also shown to significantly modify the timing response of the simulated detector.

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EAS hadronic component as registered by a neutron monitor

Cited by 8 publications

References 4 publications

Shape of spectrum of galactic cosmic ray intensity fluctuations

Shape of spectrum of galactic cosmic ray intensity fluctuations

Gadolinium loaded Cherenkov detectors for neutron monitoring in high energy air showers

Gadolinium Loaded Cherenkov Detectors for Neutron Monitoring in High Energy Air Showers

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