  The Sun has remained a difficult source to image for radio telescopes,
especially at the low radio frequencies. Its morphologically complex emission
features span a large range of angular scales, emission mechanisms involved and
brightness temperatures. In addition, time and frequency synthesis, the key
tool used by most radio interferometers to build up information about the
source being imaged is not effective for solar imaging, because many of the
features of interest are short lived and change dramatically over small
fractional bandwidths.
  Building on the advances in radio frequency technology, digital signal
processing and computing, the kind of instruments needed to simultaneously
capture the evolution of solar emission in time, frequency, morphology and
polarization over a large spectral span with the requisite imaging fidelity,
and time and frequency resolution have only recently begun to appear. Of this
class of instruments, the Murchison Widefield Array (MWA) is best suited for
solar observations. The MWA has now entered a routine observing phase and here
we present some early examples from MWA observations.
