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Observation of quasi-periodic solar radio bursts associated with propagating fast-mode waves
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Goddard, Christopher R., Nisticò, Giuseppe, Nakariakov, V. M. (Valery M.), Zimovets, I. V. and White, S. M. (2016) Observation of quasi-periodic solar radio bursts associated with propagating fast-mode waves. Astronomy & Astrophysics, 594 . A96. doi:10.1051/0004-6361/201628478 ISSN 0004-6361.
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Official URL: https://doi.org/10.1051/0004-6361/201628478
Abstract
Aims. Radio emission observations from the Learmonth and Bruny Island radio spectrographs are analysed to determine the nature of a train of discrete, periodic radio “sparks” (finite-bandwidth, short-duration isolated radio features) which precede a type II burst. We analyse extreme ultraviolet (EUV) imaging from SDO/AIA at multiple wavelengths and identify a series of quasi-periodic rapidly-propagating enhancements, which we interpret as a fast wave train, and link these to the detected radio features.
Methods. The speeds and positions of the periodic rapidly propagating fast waves and the coronal mass ejection (CME) were recorded using running-difference images and time-distance analysis. From the frequency of the radio sparks the local electron density at the emission location was estimated for each. Using an empirical model for the scaling of density in the corona, the calculated electron density was used to obtain the height above the surface at which the emission occurs, and the propagation velocity of the emission location.
Results. The period of the radio sparks, δtr = 1.78 ± 0.04 min, matches the period of the fast wave train observed at 171 Å, δtEUV = 1.7 ± 0.2 min. The inferred speed of the emission location of the radio sparks, 630 km s-1, is comparable to the measured speed of the CME leading edge, 500 km s-1, and the speeds derived from the drifting of the type II lanes. The calculated height of the radio emission (obtained from the density) matches the observed location of the CME leading edge. From the above evidence we propose that the radio sparks are caused by the quasi-periodic fast waves, and the emission is generated as they catch up and interact with the leading edge of the CME.
Item Type: | Journal Article | ||||||
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Subjects: | Q Science > QB Astronomy | ||||||
Divisions: | Faculty of Science, Engineering and Medicine > Science > Physics | ||||||
Library of Congress Subject Headings (LCSH): | Sun -- Corona, Solar oscillations, Solar radio emission | ||||||
Journal or Publication Title: | Astronomy & Astrophysics | ||||||
Publisher: | EDP Sciences | ||||||
ISSN: | 0004-6361 | ||||||
Official Date: | 18 October 2016 | ||||||
Dates: |
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Volume: | 594 | ||||||
Number of Pages: | 8 | ||||||
Article Number: | A96 | ||||||
DOI: | 10.1051/0004-6361/201628478 | ||||||
Status: | Peer Reviewed | ||||||
Publication Status: | Published | ||||||
Access rights to Published version: | Open Access (Creative Commons) | ||||||
Date of first compliant deposit: | 16 August 2016 | ||||||
Date of first compliant Open Access: | 17 May 2017 | ||||||
Funder: | European Research Council (ERC), Science and Technology Facilities Council (Great Britain) (STFC), Rossiĭskiĭ fond fundamentalʹnykh issledovaniĭ [Russian Foundation for Basic Research] (RFBR) | ||||||
Grant number: | SeismoSun Research Project No. 321141 (ERC), Grant ST/L000733/1, Grant No.15-32-21078 (RFBR) | ||||||
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