Abstract The article presents the results of solar observations during the period of high solar activity in May 2024 using the BSA LPI radio telescope. The solar corona flare activity in our data is manifested by a significant increase in the radiation flux at a frequency of 111 MHz, which is recorded not only in the main lobe of the radiation pattern, but also in distant sidelobes. The increased radio emission turns out to be highly fluctuating in time. It is shown that changes in the radio flux can lag behind changes in the coronal X-ray flux by a day or two.
Oreshko et al. (2026) studied this question.