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Fig. 5.


Panel a: NRH (solid lines) and RSTN (dashed lines) flux densities at individual frequencies from 228 to 15 400 MHz. NRH frequencies show the bump that represents the first component of the Type IV burst. Panel b: radio sources are plotted as contours at 30% and 70% levels and at three separate frequencies: 228 (orange), 327 (green), and 445 MHz (purple), and at three different times, 10:41:00 UT (left), 10:42:36 UT (middle), and 10:44:00 UT (right), denoted by dashed black lines in panel a. The radio contours are overlaid on AIA 211 Å running-difference images. Panel c: flux density spectra at NRH (red dots) and RSTN (orange triangles) frequencies at the same times as in panel b. The NRH flux densities were estimated over the northern source denoted Type IV in panel b and it excludes the southern source, which is associated with the coronal wave that is brighter. NRH fluxes are therefore lower than the RSTN fluxes.

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