  The Type-II solar radio burst recorded on 13 June 2010 by the radio
spectrograph of the Hiraiso Solar Observatory was employed to estimate the
magnetic-field strength in the solar corona. The burst was characterized by a
well pronounced band-splitting, which we used to estimate the density jump at
the shock and Alfven Mach number using the Rankine-Hugoniot relations. The
plasma frequency of the Type-II bursts is converted into height [R] in solar
radii using the appropriate density model, then we estimated the shock speed
[Vs], coronal Alfven velocity [Va], and the magnetic-field strength at
different heights. The relative bandwidth of the band-split is found to be in
the range 0.2 -- 0.25, corresponding to the density jump of X = 1.44 -- 1.56,
and the Alfven Mach number of MA = 1.35 -- 1.45. The inferred mean shock speed
was on the order of V ~ 667 km/s. From the dependencies V(R) and MA(R) we found
that Alfven speed slightly decreases at R ~ 1.3 -- 1.5. The magnetic-field
strength decreases from a value between 2.7 and 1.7 G at R ~ 1.3 -- 1.5 Rs
depending on the coronal-density model employed. We find that our results are
in good agreement with the empirical scaling by Dulk and McLean (Solar Phys.
57, 279, 1978) and Gopalswamy et al. (Astrophys. J. 744, 72, 2012). Our result
shows that Type-II band splitting method is an important tool for inferring the
coronal magnetic field, especially when independent measurements were made from
white light observations.
