  We present a detailed study of the single radio pulses of PSR B0656+14. The
emission can be characterized by two separate populations of pulses: bright
pulses have a narrow ``spiky'' appearance in contrast to the underlying weaker
broad pulses. The shape of the pulse profile requires an unusually long
timescale to achieve stability (over 25,000 pulses at 327 MHz) caused by spiky
emission. The extreme peak-fluxes of the brightest of these pulses indicates
that PSR B0656+14, were it not so near, could only have been discovered as an
RRAT source. The strongest bursts represent pulses from the bright end of an
extended smooth pulse-energy distribution, which is unlike giant pulses, giant
micropulses or the pulses of normal pulsars. Longer observations of the RRATs
may reveal that they, like PSR B0656+14, emit weaker emission in addition to
the bursts.
