The Storm of Decameter Spikes During the Event of 14 June 2012

Shevchuk, N. V.; Melnik, V.; Poedts, Stefaan; Dorovskyy, V. V.; Magdalenić, Jasmina; Konovalenko, A. A.; Браженко, А. И.; Briand, Cyril; Frantsuzenko, A. V.; Rücker, H. O.; Zarka, Philippe

doi:10.1007/s11207-015-0799-4

Cited by 23 publications

(36 citation statements)

References 17 publications

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“…The duration change with frequency may carry an important information about the plasma parameters in the emission source. Recently it was shown by Shevchuk et al [2016] that the durations of solar spikes are possibly defined by the collision times in plasma and hence can be used as a plasma temperature diagnostic tool. The durations of S-bursts are several times shorter than the collision times estimated at the corresponding heights.…”

Section: Data Analysis and Discussionmentioning

confidence: 99%

“…Their durations are considerably less than 1 s with the shortest reported value reaching 20 ms [McConnell, 1982]. The durations of other well-known short bursts, solar spikes, vary from 0.1 to 1 s at the mentioned frequencies [Shevchuk et al, 2016]. In addition Magdalenic et al [2006] reported about the super-short structures of metric type IV bursts whose durations were as small as 4 ms. S-bursts are observed exclusively at meter and decameter wavelengths [Dorovskyy et al, 2006;Melnik et al, 2010;Morosan et al, 2015].…”

Section: Introductionmentioning

confidence: 96%

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Properties of groups of solar S-bursts in the decameter band

Dorovskyy¹,

Melnik²,

Konovalenko³

et al. 2018

Planetary Radio Emissions Viii

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On 9 July 2013 from 5:30 UT till 13:28 UT more than 1000 S-bursts were recorded by the Ukrainian radio telescope UTR-2 operated in the frequency band 9-32 MHz. All S-bursts were low intensity events with an average flux of about 10 s.f.u. and a minimum flux as low as 0.2 s.f.u. which made their detection with small instruments practically impossible. New methods of observations allowed to retrieve the weakest S-bursts with fluxes comparable to the background level. The durations and frequency drift rates of these bursts as well as the dependencies of these parameters on frequency were found. The obtained results complement the analysis by Morosan et al. [2015] with data at lowest frequencies accessible for ground-based observations.

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Section: Data Analysis and Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%

Properties of groups of solar S-bursts in the decameter band

Dorovskyy¹,

Melnik²,

Konovalenko³

et al. 2018

Planetary Radio Emissions Viii

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“…The part of the dynamic spectrum with storm of spikes simultaneously with storm of Type III bursts is presented on Figure 1. This storm lasted Proceedings of Eleventh Workshop "Solar Influences on the Magnetosphere, Ionosphere and Atmosphere" Primorsko, Bulgaria, June 3÷7, 2019 during all day of observations from 04:45 up to 16:00 UT [Shevchuk N. V., et al, 2016]. The dynamic spectrum was recorded with URAN-2 coupled with new receiver DSP-Z.…”

Section: Observationsmentioning

confidence: 99%

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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“…At times of high solar activity, decameter spikes have also been observed and shown to be the low-frequency analogues of high-frequency (GHz) solar spikes used to derive the coronal plasma parameters [Shevchuk et al, 2016].…”

Section: Propagation Of Electron Beams Through the High Coronamentioning

confidence: 99%

1977-2017: 40 years of decametric observations of Jupiter and the Sun with the Nançay Decameter Array

Lamy¹,

Zarka²,

Cecconi³

et al. 2018

Planetary Radio Emissions Viii

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The Nançay Decameter Array (NDA) routinely observes low frequency (10-100 MHz) radio emissions of Jupiter and the Sun since 4 decades. The NDA observations, acquired with a variety of receivers with increasing performances, were the basis for numerous studies of Jovian and solar radio emissions and now form a unique long-term database spanning ≥ 3 solar cycles and Jovian revolutions. In addition, the NDA historically brought a fruitful support to space-based radio observatories of the heliosphere, to multi-wavelength analyses of solar activity and contributes to the development of space weather services. After having summarized the NDA characteristics, this article presents latest instrumental and database developments, some recent scientific results and perspectives for the next decade.

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The Storm of Decameter Spikes During the Event of 14 June 2012

Cited by 23 publications

References 17 publications

Properties of groups of solar S-bursts in the decameter band

Properties of groups of solar S-bursts in the decameter band

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2019

1977-2017: 40 years of decametric observations of Jupiter and the Sun with the Nançay Decameter Array

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