Abstract:
We report observations of the high frequency type II radio burst (≈430–30 MHz) that occurred in the solar corona
on 2015 November 4. The drift rate of the burst, estimated close to the start frequency of its fundamental
component (≈215 MHz), is unusually high (≈2 MHz s−1
). Our analysis shows that the estimated speed of the
magnetohydrodynamic shock driver of the burst varies with time. The peak speed and acceleration are very large,
» - 2450 km s 1 and » - 17 km s 2, respectively. There is spatio-temporal correlation between the type II burst and the
associated coronal mass ejection (CME) in the whitelight and extreme-ultraviolet images. The time profile of
the shock speed and the light curve of the associated soft X-ray flare correlate well. These results indicate that in
the present case, (i) the magnetohydrodynamic shock responsible for the high frequency coronal type II burst is
driven by the CME and (ii) the time profile of the type II burst shock speed represents the near-Sun kinematics of
the CME
