Low-frequency (80-240 MHz) radio observations of coronal holes (CHs) and type III solar radio bursts are presented using the Murchison Widefield Array (MWA). The first chapter presents a short overview of the solar corona, quiet Sun, active regions, solar flares, and CHs. The second chapter describes dark-to-bright transitions of CHs as a function of frequency. This transition is attributed to refraction of radio waves into the low density CH regions. A qualitative model is developed based on this idea and the relative optical depths. The third chapter addresses the circular polarization of type III bursts. Higher polarization fractions are found when the burst source is near disk center and lower polarization fractions are obtained near the limb. Total intensity (Stokes I), circularly polarized intensity (Stokes V), and polarization fraction (|V|/I) profiles and images of type III bursts are studied as a function of position at times near burst maximum. At burst onset, we find higher polarization fractions for the burst source, which is interpreted in terms of a larger contribution from fundamental plasma emission. At burst maximum the polarization fraction is lower, corresponding to a mixture of fundamental and harmonic emission. During the decay phase, the emission is dominated again by the fundamental component, which decays with lesser polarization fraction due to scattering. The decay time is measured, finding larger values and frequency dependences than previous observations. The fourth chapter discusses burst source sizes, flux densities, and brightness temperatures in both Stokes I and V images. The source area, fluxes and brightness temperatures increase as frequency decreases. The interpretation is that the observed changes in source size are mostly due to divergence of open magnetic field lines. The last chapter summarizes the results and suggests future work
