{"id":3350,"date":"2022-07-05T07:09:47","date_gmt":"2022-07-05T07:09:47","guid":{"rendered":"http:\/\/www.astro.gla.ac.uk\/users\/eduard\/cesra\/?p=3350"},"modified":"2022-07-05T07:09:47","modified_gmt":"2022-07-05T07:09:47","slug":"solar-radio-bursts-associated-with-in-situ-detected-energetic-electrons-in-solar-cycles-23-and-24-by-r-miteva-et-al","status":"publish","type":"post","link":"https:\/\/cesra.net\/?p=3350","title":{"rendered":"Solar radio bursts associated with in situ detected energetic\u00a0electrons in solar cycles 23 and 24 by R. Miteva et al.*"},"content":{"rendered":"

We present a short overview on the results from the first association analysis between in situ observed solar energetic electrons at 1 AU using the ACE\/EPAM instrument (<\/span>Samwel and Miteva, 2021<\/span><\/a>) and radio bursts of type II, III and IV. The statistical analysis is performed over the last two solar cycles (SCs), 23 and 24 (1997-2019). All previous research has focused on energetic protons, whereas we aimed to compare in situ electrons and remotely observed electron emission. Over the period of interest, we selected 832 electron events with identified solar origin (solar flare or\/and coronal mass ejection, CME). Radio emission signatures were identified using available dynamic radio spectra from 10 ground-based radio observatories in addition to Wind\/WAVES. Radio bursts that occur within about 1 hour after the reported solar origin onset time are selected as produced by the same solar eruption. Furthermore, the radio emissions are identified in 6 wavelength bands: dm-l (3-1 GHz), dm-h (1000-300 MHz), m-l (300-100 MHz), m-h (100-30 MHz), dam (30-3 MHz) and Hkm (3 MHz-20 kHz). No continuation of the burst (from the low corona to the interplanetary, IP, space) is implied, namely, the plots only show the individual burst appearance in the respective sub-bands.<\/span><\/p>\n

Main results<\/b><\/p>\n

Figure 1 presents the distribution of the number of type II, III and IV bursts normalized to all 832 events as a function of the radio wavelength. The wavelength trends differ among the burst types, with increasing occurrence towards the IP space for type IIIs and decreasing for type IIs and IVs.\u00a0<\/span><\/p>\n

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\nFigure 1<\/strong> – Distribution of the occurrence rate of type II, III and IV radio bursts associated with in situ electrons as a function of radio wavelength over solar cycles 23 and 24. Color code is: black – visually confirmed radio bursts, blue – uncertain identifications or observatory reports, red – data gaps in the dynamic spectra.\u00a0<\/span><\/em><\/p>\n

Some of the results in this work are summarized below:<\/span><\/p>\n