  The nonlinear evolution of Alfv\'en waves in the solar corona leads to the
generation of Alfv\'enic turbulence. This description of the Alfv\'en waves
involves parametric instabilities where the parent wave decays into slow mode
waves giving rise to density fluctuations. These density fluctuations, in turn,
play a crucial role in the modulation of the dynamic spectrum of type III radio
bursts, which are observed at the fundamental of local plasma frequency and are
sensitive to the local density. During observations of such radio bursts, fine
structures are detected across different temporal ranges. In this study, we
examine density fluctuations generated through the parametric decay instability
(PDI) of Alfv\'en waves as a mechanism to generate striations in the dynamic
spectrum of type III radio bursts using magnetohydrodynamic simulations of the
solar corona. An Alfv\'en wave is injected into the quiet solar wind by
perturbing the transverse magnetic field and velocity components which
subsequently undergo the PDI instability. The type III burst is modelled as a
fast-moving radiation source that samples the background solar wind as it
propagates to emit radio waves. We find the simulated dynamic spectrum to
contain striations directly affected by the multi-scale density fluctuations in
the wind.
