A Decameter Stationary Type Iv Burst in Imaging Observations on 2014 September 6

Koval, A. A.; Stanislavsky, A. A.; Chen, Yao; Feng, Shiwei; Konovalenko, A. A.; Volvach, Y.

doi:10.3847/0004-637x/826/2/125

Cited by 13 publications

(13 citation statements)

References 34 publications

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“…The detailed radiation mechanism was not analyzed. Our study here is distinct from that of Koval et al (2016). A IVs on September 24, 2011 is studied here.…”

Section: Introductionmentioning

confidence: 69%

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A Solar Stationary Type IV Radio Burst and Its Radiation Mechanism

et al. 2018

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A stationary Type IV (IVs) radio burst was observed on September 24, 2011. Observations from the Nançay RadioHeliograph (NRH) show that the brightness temperature (T B ) of this burst is extremely high, over 10 11 K at 150 MHz and over 10 8 K in general. The degree of circular polarization (q) is between −60% ∼ −100%, which means that it is highly left-handed circularly polarized. The flux-frequency spectrum follows a power-law distribution, and the spectral index is considered to be roughly −3 ∼ −4 throughout the IVs. Radio sources of this event are located in the wake of the coronal mass ejection and are spatially dispersed. They line up to present a formation in which lower-frequency sources are higher. Based on these observations, it is suggested that the IVs was generated through electron cyclotron maser emission.

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“…The detailed radiation mechanism was not analyzed. Our study here is distinct from that of Koval et al (2016). A IVs on September 24, 2011 is studied here.…”

Section: Introductionmentioning

confidence: 69%

“…Koval et al (2016) observed a IVs with a brightness temperature (T B ) near 10 9 K. The source region was claimed to be a "single high-lying loop" with one foot located near the active region from which the CME appeared. The detailed radiation mechanism was not analyzed.…”

Section: Introductionmentioning

confidence: 99%

A Solar Stationary Type IV Radio Burst and Its Radiation Mechanism

et al. 2018

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“…For these purposes, there must be suitable conditions. Recently, the heliographic observations of stationary type IV radio emission, done on 2014 September 6, at 16.5-33 MHz have been presented [Koval, et al, 2014]. Their analysis earnestly shows that the dynamical motion of radio sources, responsible for this event, manifests the loop response to the CME disturbance.…”

Section: Resultsmentioning

confidence: 99%

Book of Proceedings: Ninth Workshop, Sunny Beach, Bulgaria, May 30 - June 3, 2017

2017

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E Ed di it to or rs s: Katya Georgieva, Boian Kirov, Dimitar DanovProceedings of Ninth Workshop "Solar Influences on the Magnetosphere, Ionosphere and Atmosphere" Sunny Beach, Bulgaria, May 30 ÷ June 3, 2017 C C O O N N T T E E N N T T Sun and Solar Activity Podgorny I.M., Podgorny A.I. Diagnostics of Solar Flares by Analyzing the SpectralLine Emission of Highly Ionized Iron 01 Kalinichenko N., Olyak M., Konovalenko A., Brazhenko A., Ivantishin O., Lytvynenko O., Bubnov I., Yerin S., Kuhai N., Romanchuk O. A method for reconstructing the solar-wind stream structure beyond Earths orbit 07 Melnik V., Brazhenko A., Dorovskyy V., Rucker H., Panchenko M., Frantsuzenko A., Shevchuk M.. Decameter type IV burst associated with behind-limb CME observed on November 7, 2013 13 Miteva R., Samwel S.W., Krupar V. Solar radio burst emission from protonproducing flares and coronal mass ejections 19 Veselovsky I., Kaportseva K., Lukashenko A. Eight types of the solar wind and their origins 24 Stanislavsky A.A., Konovalenko A.A., Koval A.A., Volvach Ya.S.. An upgrade of the UTR-2 radio telescope to a multifrequency radio heliograph I., Gromov S.V., Kleimenova N.G., Dremukhina L.A.. Role of the IMF |Bz|/|By| in the appearance of the daytime high-latitude magnetic bays 103Proceedings of Ninth Workshop "Solar Influences on the Magnetosphere, Ionosphere and Atmosphere" Sunny Beach, Bulgaria, May 30 ÷ June 3, 2017 IV C C O O N N T T E E N N T T Solar Influences on the Lower Atmosphere and Climate Author index 133Proceedings of Ninth Workshop "Solar Influences on the Magnetosphere, Ionosphere and Atmosphere" Sunny Beach, Bulgaria, May 30 -June 3, 2017 Topic: Sun and Solar Activity Abstract.The photos of the pre-flare development observed in the spectral lines of highly ionized iron (SDO AIA apparatus) indicate the energy accumulation for a flare in the corona in the pre-flare local (about 1010 cm) high temperature structure. The pre-flare structures in the corona are observed in UV spectral lines of ions FeXXIV, FeXXIII, FeXVIII several hours before big solar flares. During a flare the emission of the UV spectral lines in the corona are increased explosively. These phenomena can be used for prediction of solar cosmic rays. Information obtained from the worldwide neutron monitor network and measurements on GOES spacecraft demonstrates unambiguously that solar cosmic rays are generated in solar flares. These phenomena are well described by the solar flare electrodynamical model, created on the basis of the observational data and the numerical magnetohydrodynamic simulation using the initial and boundary conditions, taken from the active regions observation before the flare. It is impossible to exclude that the similar mechanism of particle acceleration is responsible for galactic cosmic rays generation. Now all published mechanisms of cosmic ray generation are based on unproven assumptions. These assumptions are not confirmed by longterm observations. With the modern concept of cosmic rays, a fundamentally important qu...

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“…NDA has been used to constrain the propagation of CMEs in their early phase, and to show that it is frequently associated with electron acceleration. Prolonged electron acceleration that extends well beyond the impulsive flare phase has been observed [Carley et al, 2016;Koval et al, 2016]. The timing and frequency range determined from NDA data could be employed to trace the acceleration processes back to the interaction between the CME front and the ambient corona [Pick et al, 2016;Salas-Matamoros et al, 2016] (Figure 2 provides an illustration of the former study), e.g.…”

Section: Early Development Of Cmes and Particle Acceleration In The Cmentioning

confidence: 97%

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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A Decameter Stationary Type Iv Burst in Imaging Observations on 2014 September 6

Cited by 13 publications

References 34 publications

A Solar Stationary Type IV Radio Burst and Its Radiation Mechanism

A Solar Stationary Type IV Radio Burst and Its Radiation Mechanism

Book of Proceedings: Ninth Workshop, Sunny Beach, Bulgaria, May 30 - June 3, 2017

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

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