Neutron multiplicity: Local hadronic showers and extensive air showers

Balabin, Yu. V.; Dzhappuev, D. D.; Gvozdevsky, B. B.; Маурчев, Е. А.; Kudzhaev, A. U.; Михайлова, О. И.

doi:10.3103/s1062873811030105

Cited by 3 publications

(6 citation statements)

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“…The obtained results are important for the improvement of the recent models of induced ionization and other effects due to cosmic rays [21][22][23][24][25][26][27][28][29][30], for the various atmospheric processes (atmospheric physics and chemistry -for instance the ozone production in stratosphere [31], the…”

Section: Discussionmentioning

confidence: 99%

Cosmic ray ionization effect in the atmosphere during the maximal GLE05 − on 23.02.1956

Velinov¹,

Balabin²,

Маурчев³

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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The ground level enhancements (GLEs) due to solar cosmic rays (SCRs) are of significant astrophysical, cosmophysical and geophysical interest for a number of planetary processes on the Earth. In the present work the ionization rate profiles in the Earth's atmosphere during the outstanding ground level enhancement GLE05 on 23 February 1956, the largest one in the entire history of observations of SCRs, are obtained. The contribution of the galactic cosmic rays (GCRs) is also taken into account. The ionization in the atmosphere is calculated using the energetic spectra of solar protons, GCRs and the corresponding atmospheric cascade simulation. The spectra of solar cosmic rays are derived on the basis of ground-based measurements with neutron monitors. This method is based on solving the inverse problem -reconstruction of SCR spectrum on the boundary of the magnetosphere. The contemporary magnetosphere model "Tsyganenko 01 and 03" is used in this method. The calculation of asymptotic cones (AK) held with increments of 0.001 GV in the range of 1-20 GV. The aforementioned method is developed in the Polar Geophysical Institute (in Apatity) of the Russian Academy of Sciences. Recent simulations with RUSCOSMICS software package (based on GEANT4 program of CERN) are carried out. The energy deposit of solar protons and GCRs in the atmosphere is received. The ion production rate profiles in the stratosphere and troposphere (the region 0-40 km) are calculated for geomagnetic cut-off rigidities 1, 2, 3 and 5 GV (i.e. polar, subpolar, higher and middle latitudes, respectively). The so obtained ionization profiles are compared and thoroughly discussed. Implementations of these results are also debated. The obtained results are important for the improvement of the recent models of cosmic ray induced ionization in the whole atmosphere, for the determination of electron and ion density in the middle and lower atmosphere (troposphere), for the various atmospheric processes (as for instance in atmospheric chemistry and physicsozone production, global electric circuit between the ground and ionosphere), for the studies of solar-terrestrial influences on space weather and space climate) and for many other applications.

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Section: Discussionmentioning

confidence: 99%

Cosmic ray ionization effect in the atmosphere during the maximal GLE05 − on 23.02.1956

Velinov¹,

Balabin²,

Маурчев³

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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“…The papers Balabin et al (2010Balabin et al ( , 2011) gave a detailed survey of all the multiplicity events detected in a NM in general.…”

Section: Eas-induced Multiplicity Events In Nmmentioning

confidence: 99%

“…Criterion 3) is introduced in the present work. In Balabin et al (2011) optimal values to be used in search of MEs have been found: T 0 = 500 µs and T pau = 5000 µs. The same values are used in the present study.…”

Section: Eas-induced Multiplicity Events In Nmmentioning

confidence: 99%

“…A study has been carried out to determine in what particular part of ME the processes N 3 and N 4 occur. It has been found in Balabin et al (2010Balabin et al ( , 2011 that the average time intervals in ME don't significantly vary at the initial phase of events. But closer to the end (the final phase) of the events the time intervals increase steadily.…”

Section: Eas-induced Multiplicity Events In Nmmentioning

confidence: 99%

“…Due to the adaptability of a new high-speed data collection system, it has become possible to bind the master-pulse from the "Carpet", indicating the arrival of an EAS, to the NM pulses. A more detailed description of the data collecting system is given in Balabin et al (2009Balabin et al ( , 2010. It should be pointed out that the "Carpet" detects the EAS electronphoton component, whereas the NM detects hadrons (neutrons, protons and pions) with energy > 50 MeV (Dorman, 1975).…”

Section: Introductionmentioning

confidence: 99%

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EAS hadronic component as registered by a neutron monitor

Balabin

Gvozdevsky

Vashenyuk

et al. 2011

Astrophys. Space Sci. Trans.

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For the purposes of a study of hadron component of an extended air shower (EAS), two detectors of cosmic rays (CR) were joined at the Baksan Neutrino Observatory. They are an EAS array detector (the "Carpet") and a neutron monitor (NM). Due to the versatility of a new recording system a master-pulse, which comes from the "Carpet" and marks to occurring of EAS, is joined to NM data. After processing of the huge data set it is found that the time of EAS influence on NM is less than 1 ms. The distribution of time intervals between pulses in the first millisecond after EAS onset is essentially different from the background and shows presence of two processes with characteristic times 45 and 230 μs

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