Investigation of diurnal variations of cosmic ray fluxes measured with using ASEC and NMDB monitors

Mailyan, B.; Chilingarian, A.

doi:10.1016/j.asr.2010.01.027

Cited by 23 publications

(9 citation statements)

References 20 publications

(18 reference statements)

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“…The annual average diurnal amplitude is maximum during the declining phase of SC 23 and remains stable during the minima period of solar activity (2007)(2008)(2009), while it obtains its minimum value during 2009 (Mailyan and Chilingarian, 2010). Then, the annual average diurnal amplitude increases again during the ascending phase of SC 24.…”

Section: Diurnal Anisotropy During the Solar Cyclementioning

confidence: 75%

“…A small increase in diurnal amplitude is observed during 2005, due to various events, such as coronal mass ejections (CMEs) and magnetic storms. The amplitude is almost independent of the cut-off rigidity of the station (Bieber and Chen, 1991;Singh and Badruddin, 2006), while the amplitude variation is greater for higher-latitude stations in comparison to middle-latitude stations, such as Athens (Mailyan and Chilingarian, 2010).…”

Section: Diurnal Anisotropy During the Solar Cyclementioning

confidence: 84%

“…This can explain the long-term average, but not short-term variations in diurnal anisotropy (Yeeram and Saengdokmai, 2015). The diurnal anisotropy is also modulated by the geographic coordinates and the altitude of the detectors' location on Earth (Mailyan and Chilingarian, 2010).…”

Section: Introductionmentioning

confidence: 90%

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Latitudinal and longitudinal dependence of the cosmic ray diurnal anisotropy during 2001–2014

et al. 2016

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Abstract. The diurnal anisotropy of cosmic ray intensity for the time period 2001 to 2014 is studied, covering the maximum and the descending phase of solar cycle 23, the minimum between solar cycles 23 and 24, and the ascending phase and maximum of solar cycle 24. Cosmic ray intensity data from 11 neutron monitor stations located at different places around the Northern Hemisphere obtained from the high-resolution Neutron Monitor Database (NMDB) were used. Special software was developed for the calculations of the amplitude and the phase of the diurnal anisotropy vectors on annual and monthly basis using Fourier analysis and for the creation of the harmonic dial diagrams. The geomagnetic bending for each station was taken into account in our calculations determined from the asymptotic cones of each station via the Tsyganenko96 (Tsyganenko and Stern, 1996) magnetospheric model. From our analysis, it was resulted that there is a different behavior of the diurnal anisotropy vectors during the different phases of the solar cycles depending on the solar magnetic field polarity. The latitudinal and longitudinal distribution of the cosmic ray diurnal anisotropy was also examined by grouping the stations according to their geographic coordinates, and it was shown that diurnal variation is modulated not only by the latitude but also by the longitude of the stations. The diurnal anisotropy during strong events of solar and/or cosmic ray activity is discussed.

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Section: Diurnal Anisotropy During the Solar Cyclementioning

confidence: 75%

Section: Diurnal Anisotropy During the Solar Cyclementioning

confidence: 84%

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Latitudinal and longitudinal dependence of the cosmic ray diurnal anisotropy during 2001–2014

et al. 2016

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“…On the other hand, muons can create a considerable highenergy background for larger area detectors like PVTs (see section 4.4) when used for detecting neutroninduced high-energy gamma-rays [3]. For such detectors, diurnal variation of muon rates, cosmic neutrons and cosmic-induced gamma-rays ( [3], [18], [19]) should be considered for a complete characterization of the background in the high-energy region [3], [15].…”

Section: Cosmogenic Sourcesmentioning

confidence: 99%

Field Response Prediction: Framing the problem.

Cabrera-Palmer

2017

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“…Diurnal variations are characterized by phase and amplitude and are important data for measuring and research of the Sun -Earth interaction and the analysis of the cosmic ray fluxes (Mailyan and Chilingarian, 2010). For the period of 1 -20 November 2010, we calculated the average values of count rate for the same minute of each day.…”

Section: Data and Analysismentioning

confidence: 99%

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2018

Danov¹,

Georgieva²,

Kirov³

2018

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IIn ns st tr ru um me en nt ta at ti io on n f fo or r S Sp pa ac ce e W We ea at th he er r D Da at ta a P Pr ro oc ce es ss si in ng g a an nd d M Mo on ni it to or ri in ng g Sadovnichii V.A., Panasyuk M.I., Lipunov V.M., Bogomolov A.V., Bogomolov V.V. et.al. Monitoring of space radiation and other hazards in multi-satellite project `Universat-SOCRAT 123 S. Yerin, A. Stanislavsky, I. Bubnov, A. Konovalenko, P. Tokarsky, V. Zakharenko Small-sized radio telescopes for monitoring and studies of solar radio emission at meter and decameter wavelengths 129 M.M. Kalinichenko, O.O. Konovalenko, A.I. Brazhenko, N.V Šterc, D. Roša, D. Maričić, D. Hržina, I. Romštajn, A. Chilingarian, T. Karapetyan, D. Cafuta, M. Horvat Abstract.A powerful series of solar flares is occurred in the minimum of solar activity 2017 September 4 -11 over the active region AR12673. This active region produces two large and many small flares. The flare X8.2 is followed by solar cosmic rays. The active region at that time is situated on the back side of the Sun disk behind the Western limb. The front of the accelerated protons flux arrives to the Earth with the delay not exceeding the proton flight time from the Sun. Such proton propagation can occur only along the lines of the interplanetary magnetic field. There is no reason to believe that the mechanisms of cosmic ray acceleration on the Sun and other stars are of different nature. The flux of relativistic electrons does not show any connection with the solar cosmic rays. The results of SDO spacecraft are used to study the pre-flare state and flare development. The source of flare radiation in the spectral lines of the highly ionized irons FeXXIV and FeXXIII is observed in the corona. The emission of these spectral lines sharp increases during flare X-ray radiation appearing. The energy release of a flare occurs in the corona above an active region. The temperature in the flare is greater than 20 MK. The size of the hot plasma cloud is ~10 10 cm. IntroductionThe solar constant indicates an amazing stability of the solar thermonuclear reactor. The solar constant is 1367 W/m 2 . The change of the solar constant during the 11-year cycle of solar activity does not exceed ~10 -3 . Against the backdrop of this amazing stability of the Sun's work the big solar flares are observed several times per a year. The flare energy release takes place in the corona over a complex active region with a magnetic flux greater than 10 22Mx. The energy of a solar flare can exceed 10 32 erg. The flare duration is from 10 to 100 minutes. The flare is a manifestation of a number of physical processes, including X-ray radiation, the ejection of the corona substance and proton acceleration to the relativistic energy of not less than 20 GeV [Balabin et al., 2005; Podgorny and Podgorny, 2016].The Sun is the only astronomical object that generates proton pulses with the relativistic energy. The solar proton acceleration takes place along a singular line of the current sheet above an active region. The electric ...

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Investigation of diurnal variations of cosmic ray fluxes measured with using ASEC and NMDB monitors

Cited by 23 publications

References 20 publications

Latitudinal and longitudinal dependence of the cosmic ray diurnal anisotropy during 2001–2014

Latitudinal and longitudinal dependence of the cosmic ray diurnal anisotropy during 2001–2014

Field Response Prediction: Framing the problem.

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2018

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