Coronal Sources of the Solar F10.7 Radio Flux

We present results from the first solar full-disk {{{F}}}_10.7 (the radio flux at 10.7 cm, 2.8 GHz) image taken with the S-band receivers on the recently upgraded Karl G. Jansky Very Large Array in order to assess the relationship between the {{{F}}}_10.7 index and solar extreme ultraviolet (EUV) emission. To identify the sources of the observed 2.8 GHz emission, we calculate differential emission measures from EUV images collected by the Atmospheric Imaging Assembly and use them to predict the bremsstrahlung component of the radio emission. By comparing the bremsstrahlung prediction and radio observation we find that 8.1% ± 0.5% of the variable component of the {{{F}}}_10.7 flux is associated with the gyroresonance emission mechanism. Additionally, we identify optical depth effects on the radio limb which may complicate the use of {{{F}}}_10.7 time series as an EUV proxy. Our analysis is consistent with a coronal iron abundance that is four times the photospheric level.