  We report a solar coronal split-band type II radio burst that was observed on
2016 March 16 with the Gauribidanur Radio Spectro-Polarimeter (GRASP) in the
frequency range $\approx$\,90\,-\,50 MHz, and the Gauribidanur RadioheliograPH
(GRAPH) at two discrete frequencies, viz. 80 MHz and 53.3 MHz. Observations
around the same epoch in extreme-ultraviolet (EUV) and white-light show that
the above burst was associated with a flux rope structure and a coronal mass
ejection (CME), respectively. The combined height-time plot generated using
EUV, radio, and whitelight data suggest that the different observed features
(i.e. the flux rope, type II burst and the CME) are all closely associated. We
constructed an empirical model for the coronal electron density distribution
($N_{e}(r)$, where $r$ is the heliocentric distance) from the above set of
observations themselves and used it to estimate the coronal magnetic field
strength ($B$) over the range of $r$ values in which the respective events were
observed. The $B$ values are consistent with each other. They vary as
$B(r)\,=\,2.61 \times r^{-2.21}$ \textrm{G} in the range $r
\approx$\,1.1\,-\,2.2$\rm R_{\odot}$. As far as we know, similar `direct'
estimates of $B$ in the near-Sun corona without assuming a model for
$N_{e}(r)$, and by combining co-temporal set of observations in two different
regions (radio and whitelight) of the electromagnetic spectrum, have rarely
been reported. Further, the present work is a novel attempt where the
characteristics of a propagating EUV flux rope structure, considered to be the
signature of a CME close the Sun, have been used to estimate $B(r)$ in the
corresponding distance range.
