Scientific Set of Instruments “Solar Cosmic Rays”

Kuznetsov, S. N.; Bogomolov, A. V.; Галкин, В. И.; Denisov, Yu. I.; Podorolsky, A. N.; Ryumin, S. P.; Kudela, K.; Rojko, J.

doi:10.1007/978-3-642-39268-9_9

Cited by 4 publications

(7 citation statements)

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“…It consists of CsJ crystal of 10 mm diameter and height. CsJ has a higher density comparing with Si-detectors and allows to measure electrons with higher energy [Kuznetsov et al, 2014]. Different colors represent events depending on the localization of the SEP-related solar flare on the solar disk according to the SOHO/ERNE catalog: west events (W90-W30 degrees) in red color, central events (W30-E30 degrees) -green, east events (E30-E90 degrees) -oblique crosses.…”

Section: Summary and Discussionmentioning

confidence: 99%

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Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2019

Nikitenko¹,

Lebed²,

Fedorenko³

et al. 2019

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The Catalogues of the solar proton events [Logachev, ed., 1982-2016] provide the homogeneous data series of events with maximum intensity of > 10 MeV solar protons J ≥ 1 cm-2 s-1 sr-1 beginning from 1970 up to now. The event rates behavior is rather smooth: the total number of such events, relative to accumulated sunspot number, is almost constant in the solar cycles 21-23 and even slightly growing in the solar cycle 24. Contrary, the total number of the most powerful (GLE) events per cycle was constant within statistical errors in the cycles 21-23, and it fell abruptly in cycle 24. Considering the conventional sources of GLEs we found that production of GLEs by X-class bursts was 3 times less in cycle 24 than in cycle 23, while production of GLEs by the >1000 km/s halo-type CMEs was 5 times lower.

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Section: Summary and Discussionmentioning

confidence: 99%

“…Thus, the period of selection should be limited by the observation of one instrument observing in this spectral region. We used data by CORONAS/SONG spacecraft for the period 2001-2005 [Kuznetsov et al, 2014]. This instrument obtained 1D and spectral observations but with high sensitivity to weak fluxes in non-thermal X-ray range.…”

Section: Proceedings Ofmentioning

confidence: 99%

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2019

Nikitenko¹,

Lebed²,

Fedorenko³

et al. 2019

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“…that based on [59] with high flexibility) and γ ray monitoring detector (using e.g. experience from CORONAS-F [60]) and to coordinate the JEM-EUSO observations with other satellites targeted to ionospheric/magnetospheric phenomena research as well as with ground based CR measurements, especially on mountains.…”

Section: Discussionmentioning

confidence: 99%

Possibilities for selected space weather and atmospheric studies in JEM-EUSO project?

Kudela¹

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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for the JEM-EUSO CollaborationThe main scientific task of JEM-EUSO is to observe the ultra high energy cosmic rays by looking the atmosphere from space [1,2,3,4]. The detailed description of various sources of the background is important. On the other hand, the study of selected magnetospheric, ionospheric and atmospheric processes related to temporal and spatial variability of UV (ultraviolet) on the orbit where JEM-EUSO is supposed to be situated, could be a useful by-product of the main task of the project (e.g. review [5]). We attempt to summarize selected processes connected with atmospheric electricity and with energetic particles having links to the events as TLE (transient luminous event), TGF (terrestrial gamma-ray flash) and TGE (thunderstorm ground enhancement), recently observed on mountains too. Our groups (in CBK Warsaw, in IEP Košice) have a long track of experience with measurements of waves and particles for magnetospheric/ionospheric research as well as with physical analysis/interpretation of the data obtained. The JEM-EUSO, if the experiment is augmented by a very simple device that monitors energetic particles, and coordinated with other satellite measurements and with ground based observations, may be of relevance for some space weather studies related to the effects in the chain magnetosphere/ionosphere/atmosphere. This can contribute to better understanding of electromagnetic responses of lightning on the Earth and of selected processes at high altitudes in the atmosphere.

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“…At the beginning of its flight CORONAS-F had a quasicircular orbit, with initial parameters: altitude 507±21 km, inclination 82.5 degrees, and period of revolution 94.5 min. The primary goal of the CORONAS-F experiment was to investigate nonstationary processes on the Sun and their impact on the interplanetary medium and the Earth's magnetosphere [Kuznetsov et al, 2014].The development of a complex program of the studies of solar activity and its influence on the near-Earth space began in the USSR in the middle of 80s years of the 20th century. It resulted in a development of a number of satellites of CORONAS series.…”

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“…Amplitude of impulse produced by the charged particle is measured by scintillator detector, for the further analysis the particles with energy release in "n-p" detector exceeding double ionization of a relativistic single-charged particle are selected. The detailed description of SONG and MKL instruments is given in [Kuznetsov et al, 2014]. In addition, data from the Radio Solar Telescope Network (RSTN) is used for investigating the behavior of the temporal profiles of the radio emission.…”

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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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Scientific Set of Instruments “Solar Cosmic Rays”

Cited by 4 publications

References 2 publications

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2019

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2019

Possibilities for selected space weather and atmospheric studies in JEM-EUSO project?

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2018

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