A Solar Stationary Type IV Radio Burst and Its Radiation Mechanism

Abstract

A stationary Type IV (IVs) radio burst was observed on September 24, 2011. Observations from the Nançay RadioHeliograph (NRH) show that the brightness temperature ( $T_{\mathrm{B}}$ ) of this burst is extremely high, over $10^{11}$ K at 150 MHz and over $10^{8}$ K in general. The degree of circular polarization ( $q$ ) is between $-60\% \sim -100\%$ , which means that it is highly left-handed circularly polarized. The flux–frequency spectrum follows a power-law distribution, and the spectral index is considered to be roughly $-3 \sim -4$ throughout the IVs. Radio sources of this event are located in the wake of the coronal mass ejection and are spatially dispersed. They line up to present a formation in which lower-frequency sources are higher. Based on these observations, it is suggested that the IVs was generated through electron cyclotron maser emission.