  A high-speed halo-type coronal mass ejection (CME), associated with a GOES
M4.6 soft X-ray flare in NOAA AR 0180 at S12W29 and an EIT wave and dimming,
occurred on 9 November 2002. A complex radio event was observed during the same
period. It included narrow-band fluctuations and frequency-drifting features in
the metric wavelength range, type III burst groups at metric--hectometric
wavelengths, and an interplanetary type II radio burst, which was visible in
the dynamic radio spectrum below 14 MHz. To study the association of the
recorded solar energetic particle (SEP) populations with the propagating CME
and flaring, we perform a multi-wavelength analysis using radio spectral and
imaging observations combined with white-light, EUV, hard X-ray, and
magnetogram data. Velocity dispersion analysis of the particle distributions
(SOHO and Wind in situ observations) provides estimates for the release times
of electrons and protons. Our analysis indicates that proton acceleration was
delayed compared to the electrons. The dynamics of the interplanetary type II
burst identify the burst source as a bow shock created by the fast CME. The
type III burst groups, with start times close to the estimated electron release
times, trace electron beams travelling along open field lines into the
interplanetary space. The type III bursts seem to encounter a steep density
gradient as they overtake the type II shock front, resulting in an abrupt
change in the frequency drift rate of the type III burst emission. Our study
presents evidence in support of a scenario in which electrons are accelerated
low in the corona behind the CME shock front, while protons are accelerated
later, possibly at the CME bow shock high in the corona.
