On ionization in the ionospheric D-region by galactic and solar cosmic rays

Velinov, P.

doi:10.1016/0021-9169(68)90031-7

Cited by 67 publications

(29 citation statements)

References 7 publications

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“…Over 50 years ago were made calculations of ionization profiles q(h) in the lower ionosphere (50-100 km) due to the penetration of relativistic SEPs during the GLE05 on February 23, 1956 [5][6][7][8][9]. In the atmosphere cosmic particles enter in electromagnetic and nuclear interactions with the substance of the air.…”

Section: Earlier Results For Enhanced Ionization In Ionosphere Duringmentioning

confidence: 99%

“…In the atmosphere cosmic particles enter in electromagnetic and nuclear interactions with the substance of the air. The first results for q(h) profiles [5][6][7][8][9] were obtained without accounting the nuclear interactions between the secondary cosmic ray particles and the Earth's atmosphere, which is quite acceptable for these altitudes. In the ionospheric D-region (50-100 km) the predominant interactions are the electromagnetic due to the small atmospheric depth (less than 1 g/cm 2 ) for the cosmic ray particles [7].…”

Section: Earlier Results For Enhanced Ionization In Ionosphere Duringmentioning

confidence: 99%

“…The GCRs create the continuous and permanent ionization in the atmosphere, and also the independent ionospheric cosmic ray layer (CR layer) at altitudes 50-80 km in the D region in the lower ionosphere [5,[7][8][9]]. Yet in [5,7] are made some calculations of the electron production and electron density in the CR layer.…”

Section: Comparisson To Other Resultsmentioning

confidence: 99%

“…That's why after receiving the initial results [5][6][7][8][9] were made calculations taking into account all nuclear reactions [10][11][12]. One possible tool is based on Monte Carlo simulation of the cascade process in the atmosphere, precisely the energy deposit and afterwards the estimation of ion pair production.…”

Section: Previous Computations For Ionization In Strato-troposphere Dmentioning

confidence: 99%

“…The specific formula (1) refers to the middle latitudes -geomagnetic cutoff rigidity ≈ 5 GV and an average solar activity. The differential spectrum of SCRs generally has the following description [6,7,10]:…”

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confidence: 99%

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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: Earlier Results For Enhanced Ionization In Ionosphere Duringmentioning

confidence: 99%

Section: Earlier Results For Enhanced Ionization In Ionosphere Duringmentioning

confidence: 99%

Section: Comparisson To Other Resultsmentioning

confidence: 99%

Section: Previous Computations For Ionization In Strato-troposphere Dmentioning

confidence: 99%

mentioning

confidence: 99%

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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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Modeling of long‐path propagation characteristics of VLF radio waves as observed from Indian Antarctic station Maitri

2015

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Propagation of very low frequency (VLF) radio signal through the Earth‐ionosphere waveguide depends strongly on the plasma properties of the ionospheric D layer. Solar extreme ultraviolet radiation plays the central role in controlling physical and chemical properties of the lower ionospheric layers and hence determining the propagation characteristics of a VLF signal. The nature of interference among different propagating modes varies widely with the length of the propagation path. For a very long path, exposure of solar radiation and thus the degree of ionization vary by a large amount along the path. This influences the VLF signal profile by modulating the sky wave propagation. To understand the propagation characteristics over such a long path, we need a thorough investigation of the chemical reactions of the lower ionosphere which is lacking in the literature. Study of radio signal characteristics in the Antarctic region during summer period in the Southern Hemisphere gives us a unique opportunity to explore such a possibility. In addition, there is an extra feature in this path—the presence of solar radiation and hence the D region for the whole day during summer in at least some sections of the path. In this paper, we present long‐distance propagation characteristics of VLF signals transmitted from VTX (18.2 kHz) and NWC (19.8 kHz) transmitters recorded at the Indian permanent station Maitri (latitude 70° 45′S, longitude 114° 40′E) in 2007–2008. A very stable diurnal variation of the signal has been obtained with no signature of nighttime fluctuation due the presence of 24 h of sunlight. Using ion production and recombination profiles by solar irradiance and incorporating D region ion chemistry processes, we calculate the electron density profile at different heights. Using this profile in the Long Wavelength Propagation Capability code, we are able to reproduce the amplitude of VLF signal.

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Photochemical response of the nighttime mesosphere to electric field heating—Onset of electron density enhancements

Kotovsky

Moore

2016

JGR Space Physics

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Onsets of electron density enhancements in the upper nighttime mesosphere produced by electric field heating of electrons are examined using a photochemical model that accounts for 29 dynamic species via a set of 156 reactions. Physical mechanisms are identified which result in electron density enhancements that continuously increase for up to several seconds after electric field heating, establishing the conditions under which early VLF scattering is either “fast” (<20 ms) or slower(>20 ms, including “slow,” ≥500 ms). During heating, O− ions are produced by heterolysis, e− + O2 → e− + O− + O+, and dissociative attachment, e−+ O2 → O− + O. Following heating, a significant proportion of O− ions associatively detach with molecular oxygen, O− + O2 → O3 + e−, and atomic oxygen, O− + O → O2 + e−. If enough O− ions are produced during heating such that O− detachment exceeds electron loss (predominantly attachment, e− + O3 → normalO2− + O, and/or electron‐ion recombination), electron densities will continue to increase after heating has ended. Consequently, the total risetime of electron density enhancements produced by electric field heating is controlled by the duration of the electric field heating and (in some cases) the effects of O− detachment following heating.

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On ionization in the ionospheric D-region by galactic and solar cosmic rays

Cited by 67 publications

References 7 publications

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

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

Modeling of long‐path propagation characteristics of VLF radio waves as observed from Indian Antarctic station Maitri

Photochemical response of the nighttime mesosphere to electric field heating—Onset of electron density enhancements

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