  We report spectral and polarimeter observations of two weak, low frequency
(${\approx}$85-60\,MHz) solar coronal type II radio bursts that occurred on
2020 May 29 within a time interval ${\approx}$2\,min. The bursts had fine
structures, and were due to harmonic plasma emission. Our analysis indicates
that the magnetohydrodynamic (MHD) shocks responsible for the 1st and 2nd type
II bursts were generated by the leading edge (LE) of an extreme-ultraviolet
(EUV) flux rope/coronal mass ejection (CME) and interaction of its flank with a
neighbouring coronal structure, respectively. The CME deflected from the radial
direction by ${\approx}25^{\arcdeg}$ during propagation in the near-Sun corona.
The estimated power spectral density (PSD) and magnetic field strength ($B$)
near the location of the 1st burst at heliocentric distance
$r{\approx}1.35R_{\odot}$ are $\rm {\approx}2{\times}10^{-3}\,W^{2}m$ and
${\approx}$1.8\,G, respectively. The corresponding values for the 2nd burst at
the same $r$ are $\rm {\approx}10^{-3}\,W^{2}m$ and ${\approx}$0.9\,G. The
significant spatial scales of the coronal turbulence at the location of the two
type II bursts are ${\approx}$62\,-\,1\,Mm. Our conclusions from the present
work are that the turbulence and magnetic field strength in the coronal region
near the CME LE are higher compared to the corresponding values close to its
flank. The derived estimates of the two parameters correspond to the same $r$
for both the CME LE and its flank, with a delay of ${\approx}$2\,min for the
latter.
