Fig. 1 | Nature Communications

Fig. 1

From: Loss-cone instability modulation due to a magnetohydrodynamic sausage mode oscillation in the solar corona

Fig. 1The alternative text for this image may have been generated using AI.

EUV and radio imaging of the flare and quiet active regions. a Extreme ultraviolet running ratio images from the SDO AIA 21.1 and 17.1 nm passbands overlaid with NRH 228 MHz contours. The flare AR is responsible for the majority of radio activity during the event, such as Source 1. b In a quiet AR approximately 400 Mm (600 arcseconds) east of the flare site, a second radio Source 2 appears. This quiet AR shows signs of disturbed coronal loops (as indicated) at the time of Source 2. Source 2 shows periodic variations in flux density for up to 2.5 min, shown in Fig. 2 below

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