Comparative analysis of the proton generation efficiency during 17 March 2003 and 11 April 2004 solar flares

Bogomolov, A. V.; Myagkova, I. N.; Myshyakov, I. I.; Tsvetkov, Ts.; Kashapova, L. K.; Miteva, R.

doi:10.1016/j.jastp.2018.08.010

Cited by 3 publications

(6 citation statements)

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“…During the flight, the threshold values slowly increased, by the end of 2005 the difference was about 1.5 times. A more detailed description of the experiments with SPR-N and SONG can be found in earlier works [Bogomolov et al 2003, Bogomolov and Myagkova 2017, Zhitnik et al 2006. Table 1 List of solar flares observed by the SPR-N instrument which can be used to separate the thermal and non-thermal components of X-ray radiation.…”

Section: Discussionmentioning

confidence: 99%

“…In the comparative analysis of flares with similar characteristics, but with different geoeffectiveness, it was shown that it may be important to take into account the conditions for the release of particles from the flare area (magnetic field topology) [Bogomolov et al, 2018]. The same conditions can affect how much of the energy of the accelerated electrons will be used to heat the solar plasma, and which will leave the flare region along with the accelerated particles.…”

Section: Introductionmentioning

confidence: 99%

“…But on the other hand, weak flares may be associated with prominent SEP events. In the work by Bogomolov et al [2018] a comparison between the characteristics of two flares was carried out. These flares show very close characteristics of the acceleration processes.…”

Section: Introductionmentioning

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: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2019

Nikitenko¹,

Lebed²,

Fedorenko³

et al. 2019

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“…We analyzed the SEP events associated with the solar flares that occurred on August 20 and 24, 2002, March 17, 2003, April 11, 2004, January 17 and 20, 2005. Table 1 presents data on six solar flares detected by SONG instrument on board CORONAS-F satellite.…”

Section: Datamentioning

confidence: 99%

“…This fact could be related with features of active regions (ARs) which were not taken into account in this study. In the paper of Bogomolov et al [2018] to the analysis of SEP fluxes and flare plasma parameters were added also studies of the magnetic topology of the AR and its evolution before and during the solar flares. The presented results indicate that an arcade of high loops covering the AR could prevent escaping of the accelerated particles and generates a less proton-rich SEP event as it is expected by flare properties alone.…”

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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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Technical performance and first light of the new 1.5-meter telescope at the National Astronomical Observatory Rozhen

Minev,

Petrov,

Semkov

2024

caosp

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A new 1.5-meter Ritchey-Chretien telescope has been inaugurated as part of the observational equipment of the Institute of Astronomy and the National Astronomical Observatory Rozhen (IANAO) at the Bulgarian Academy of Science (BAS). The telescope, designed with advanced optical and mechanical components, aims to enhance observational capabilities from NAO Rozhen. Here, we present the initial tests and setup procedures conducted for the new telescope and we describe the assembly process, alignment procedures, and calibration techniques implemented to ensure optimal performance. The tests involved nighttime observations and preliminary results highlight the successful alignment of the telescope's optics, the stability of its tracking mechanism, and the establishment of an efficient data acquisition workflow. The findings from these initial tests provide valuable insights into the telescope's capabilities and help us to set up a fully robotic telescope for observational campaigns and scientific research. This new observational instrument will primarily perform photometric and astrometric tasks. However, there is also the possibility of conducting low-dispersion spectral observations.

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Comparative analysis of the proton generation efficiency during 17 March 2003 and 11 April 2004 solar flares

Cited by 3 publications

References 40 publications

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2019

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2019

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2018

Technical performance and first light of the new 1.5-meter telescope at the National Astronomical Observatory Rozhen

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