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Observations of solar radio burst fine structures with LOFAR by E. Kontar et al.*

28 Nov 2017, 10:05 UTC
Observations of solar radio burst fine structures with LOFAR  by E. Kontar et al.* NASA/Goddard/SDO
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During solar flares, electrons are accelerated up to relativistic speeds. As they propagate upwards through the solar corona, they produce so-called type III radio bursts. These type III bursts often demonstrate fine structure, with their spectra consisting of multiple narrowband “striae”; most likely, these structures are caused by small-scale density inhomogeneities of the coronal plasma so that the subsequent fundamental plasma processes that produce the radio bursts is produced in small localized regions (e.g. Takakura & Yousef, 1975; Melrose & Goldman, 1987; Kontar, 2001).
Using one of the largest radio telescopes, the LOw Frequency ARray (LOFAR, van Haarlem et al. 2013), we have estimated the source sizes and locations of the fine frequency structures in the solar radio burst. Utilizing high time resolution (~10 ms) and frequency resolution (12 kHz), we have also determined the location and size of the radio emission source (Figure 1) and its evolution with time, allowing us to track how the radio emission propagates through the solar corona.

Figure 1. Radio images of the fine structure components of the burst. Superimposed images of the Extreme Ultra-Violet (EUV) image from SDO. Green: Observations from the Solar Dynamics Observatory/Atmospheric Imaging Assembly 171 Å at 2015 April 16 ...

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