Faint solar radio structures from decametric observations

Briand, Cyril; Zaslavsky, A.; Maksimović, M.; Zarka, Philippe; Lecacheux, A.; Rücker, H. O.; Konovalenko, A. A.; Abranin, E. P.; Dorovsky, V. V.; Stanislavsky, A. A.; Melnik, V. N.

doi:10.1051/0004-6361:200809842

Cited by 18 publications

(15 citation statements)

References 18 publications

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“…The distribution is evidently asymmetric, with a steep slope towards slower drift rates and a rather flat fall towards faster ones. This distribution resembles those obtained for forward drift pairs (Melnik et al, 2005) and solar S-bursts (Dorovskyy et al, 2006;Briand et al, 2008).…”

Section: Frequency Drift Rates Of the Hb Sub-burstssupporting

confidence: 84%

Fine and Superfine Structure of the Decameter–Hectometer Type II Burst on 7 June 2011

et al. 2015

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The characteristics of a type II burst with a herringbone structure observed both with ground-based radio telescopes (UTR-2 and URAN-2) and space-borne spectrometers (STEREO-A and B) are discussed. The burst was recorded on 7 June 2011 in the frequency band 3 -33 MHz. It was characterized by extremely rich fine structure. Statistical analysis of more than 300 herringbone sub-bursts constituting the burst was performed separately for the positively (reverse) and negatively (forward) drifting sub-bursts. The sense and the degree of circular polarization of the herringbone sub-bursts were measured in a wide frequency band (16 -32 MHz). A second-order fine frequency structure of the herringbone sub-bursts was observed and studied for the first time. Using STEREO/COR1 and SOHO/LASCO-C2 images, we determined the direction and radial speed of the coronal mass ejection responsible for the studied type II burst. The possible location of the type II burst source on the flank of the shock was found.

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Section: Frequency Drift Rates Of the Hb Sub-burstssupporting

confidence: 84%

Fine and Superfine Structure of the Decameter–Hectometer Type II Burst on 7 June 2011

et al. 2015

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“…In addition, these bursts remind one of Jovian S-bursts by their dynamic spectra. Solar S-bursts are narrow tracks, which drift from high to low frequencies against the background of other solar radio activities as pointed out by various authors (Ellis, 1969;McConnell and Ellis, 1981;McConnell, 1982;Barrow, Zarka, and Aubier, 1994;Dorovskyy et al, 2006;Briand et al, 2008). In rare cases S-bursts have positive drift (from low to high frequencies) (McConnell, 1982).…”

Section: Introductionmentioning

confidence: 90%

Solar S-bursts at Frequencies of 10 – 30 MHz

Melnik¹,

Konovalenko²,

Rücker³

et al. 2010

Sol Phys

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Solar S-bursts observed by the radio telescope UTR-2 in the period 2001 -2002 are studied. The bursts chosen for a detailed analysis occurred in the periods 23 -26 May 2001, 13 -16 and 27 -39 July 2002 during three solar radio storms. More than 800 S-bursts were registered in these days. Properties of S-bursts are studied in the frequency band 10 -30 MHz. All bursts were always observed against a background of other solar radio activity such as type III and IIIb bursts, type III-like bursts, drift pairs and spikes. Moreover, Sbursts were observed during days when the active region was situated near the central meridian. Characteristic durations of S-bursts were about 0.35 and 0.4 -0.6 s for the May and July storms, respectively. For the first time, we found that the instantaneous frequency width of S-bursts increased with frequency linearly. The dependence of drift rates on frequency followed the McConnell dependence derived for higher frequencies. We propose a model of S-bursts based on the assumption that these bursts are generated due to the confluence of Langmuir waves with fast magnetosonic waves, whose phase and group velocities are equal.

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“…As solar type II and III radio bursts are emitted at 1-2 times the plasma frequency (such as on shock fronts at stream interfaces in the solar wind, coronal mass ejections, and by energetic electron beams), occurrence and evolution of these structures would be monitored throughout the solar corona. Goniopolarimetry would provide directional information on the emitting structures [12], and Farside Explorer observations would be used synergistically with spacecraft observations at similar frequencies and ground-based observations at higher frequencies [8].…”

Section: Radio Astronomymentioning

confidence: 99%

Farside explorer: unique science from a mission to the farside of the moon

et al. 2011

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Farside Explorer is a proposed Cosmic Vision medium-size mission to the farside of the Moon consisting of two landers and an instrumented relay satellite. The farside of the Moon is a unique scientific platform in that it is shielded from terrestrial radio-frequency interference, it recorded the primary differentiation and evolution of the Moon, it can be continuously monitored from the Earth-Moon L2 Lagrange point, and there is a complete lack of reflected solar illumination from the Earth. Farside Explorer will exploit these properties and make the first radio-astronomy measurements from the most radio-quiet region of near-Earth space, determine the internal structure and thermal evolution of the Moon, from crust to core, and quantify impact hazards in near-Earth space by the measurement of flashes generated by impact events. The Farside Explorer flight system includes two identical solarpowered landers and a science/telecommunications relay satellite to be placed in a halo orbit about the Earth-Moon L2 Lagrange point. One lander would explore the largest and oldest recognized impact basin in the Solar SystemExp Astron (2012) 33:529-585 531 the South Pole-Aitken basin-and the other would investigate the primordial highlands crust. Radio astronomy, geophysical, and geochemical instruments would be deployed on the surface, and the relay satellite would continuously monitor the surface for impact events.

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Faint solar radio structures from decametric observations

Cited by 18 publications

References 18 publications

Fine and Superfine Structure of the Decameter–Hectometer Type II Burst on 7 June 2011

Fine and Superfine Structure of the Decameter–Hectometer Type II Burst on 7 June 2011

Solar S-bursts at Frequencies of 10 – 30 MHz

Farside explorer: unique science from a mission to the farside of the moon

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