  During non-flaring times, the radio flux of the Sun at the wavelength of a
few centimeters to several tens of centimeters mostly originates from the
thermal bremsstrahlung emission, very similar to the EUV radiation. Owing to
such a proximity, it is feasible to investigate the relationship between the
EUV emission and radio emission in a quantitative way. In this paper, we
reconstruct the radio images of the Sun through the differential emission
measure obtained from the multi-wavelength EUV images of the Atmospheric
Imaging Assembly on board Solar Dynamic Observatory. Through comparing the
synthetic radio images at 6 GHz with those observed by Siberian
Radioheliograph, we find that the predicted radio flux is qualitatively
consistent with the observed value, confirming thermal origin of the coronal
radio emission during non-flaring times. The results further show that the
predicted radio flux is closer to the observations in the case of including the
contribution of the plasma with temperatures above 3 MK than in the case of
only involving the low temperature plasma as was usually done in the era of
pre-SDO. We also discuss the applications of the method and uncertainties of
the results.
