  Low-frequency (80-240 MHz) radio observations of the solar corona are
presented using the Murchison Widefield Array (MWA), and several discoveries
are reported. The corona is reviewed, followed by chapters on Type III bursts
and circularly-polarized quiescent emission. The second chapter details new
Type III burst dynamics. One source component at higher frequencies splits into
two at lower frequencies, where the two components rapidly diverge. This is
attributed to electron beams traversing a divergent magnetic field
configuration, which is supported by extreme ultraviolet jet observations
outlining a coronal null point. The third chapter uses Type III burst heights
as density probes. Harmonic plasma emission implies ~4x enhancements over
background models. This can be explained by electron beams traveling along
dense fibers or by propagation effects that elevate apparent source heights.
The quiescent corona is compared to model predictions to conclude that
propagation effects can largely but not entirely explain the apparent density
enhancements. The fourth chapter surveys over 100 spectropolarimetric observing
runs. Around 700 compact sources are detected with polarization fractions from
less than 0.5% to nearly 100%. They are interpreted as plasma emission noise
storm sources down to levels not previously observable. A "bullseye" structure
is reported for coronal holes, where an outer ring surrounds an
oppositely-polarized central component that does not match the sign expected of
thermal bremsstrahlung. The large-scale polarization structure is shown to be
well-correlated with that of a global magnetic field model. The last chapter
summarizes results and outlines future work. A preliminary comparison of
polarization images to model predictions is shared, along with coronal mass
ejection observations revealing a radio arc that is morphologically similar to
the white-light structure.
