The curves to the left show the temporal evolution of the solar radio flux at five frequencies, between 329 and 870 MHz (resp. 91 and 34 cm of wavelength). The data are collected with a 6m dish from the Humain Radioastronomy Station, whose realtime pointing and picture are shown below.

The different radio light curves show the rise of the Sun, around 07:30UT (08:30 Local Time), while the telescope is pointing towards the East. It then starts tracking the Sun until approximately 16:00UT (17:00LT). The ripples seen on the curves are due to the solar radiation reflecting on the ground and interfering with the one directly collected by the telescope parabola. Spikes on the curves are either solar bursts (especially if they appear on different curves at the same time) or interference.

During the eclipse, the flux decreases as the Moon passes in front of the Sun. The radio Sun is more extended than the optical one because the radio emission at these frequencies originates from outer layers of the solar atmosphere (corona). Therefore, the radio eclipse will last a bit longer than the optical one.

The corona is not uniform due to active regions and other large scale coronal structures. The drop and increase of the intensity curve is not proportional to the solar atmosphere covered by the Moon, and can therefore be a-symmetric.