Low frequency radio observations of bi-directional electron beams in the solar corona

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20153801294931
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[1] [1,Carley, Eoin P.
[2] Reid, Hamish
[3] Vilmer, Nicole
[4] Gallagher, Peter T.
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| 1600年 / EDP Sciences卷 / 581期
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The radio signature of a shock travelling through the solar corona is known as a type II solar radio burst. In rare cases these bursts can exhibit a fine structure known as herringbones; which are a direct indicator of particle acceleration occurring at the shock front. However; few studies have been performed on herringbones and the details of the underlying particle acceleration processes are unknown. Here; we use an image processing technique known as the Hough transform to statistically analyse the herringbone fine structure in a radio burst at ∼20-90 MHz observed from the Rosse Solar-Terrestrial Observatory on 2011 September 22. We identify 188 individual bursts which are signatures of bi-directional electron beams continuously accelerated to speeds of 0.16-0.10+0.11c. This occurs at a shock acceleration site initially at a constant altitude of ∼0.6 Ro in the corona; followed by a shift to ∼0.5 Ro. The anti-sunward beams travel a distance of 170-97+174 Mm (and possibly further) away from the acceleration site; while those travelling toward the Sun come to a stop sooner; reaching a smaller distance of 112-76+84 Mm. We show that the stopping distance for the sunward beams may depend on the total number density and the velocity of the beam. Our study concludes that a detailed statistical analysis of herringbone fine structure can provide information on the physical properties of the corona which lead to these relatively rare radio bursts. © ESO; 2015;
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