  The Sun produces the most powerful explosions in the solar system, solar
flares, that can also be accompanied by large eruptions of magnetised plasma,
coronal mass ejections (CMEs). These processes can accelerate electron beams up
to relativistic energies through magnetic reconnection processes during solar
flares and CME-driven shocks. Energetic electron beams can in turn generate
radio bursts through the plasma emission mechanism. CME shocks, in particular,
are usually associated with type II solar radio bursts. However, on a few
occasions, type II bursts have been reported to occur either in the absence of
CMEs or shown to be more likely related with the flaring process. It is
currently an open question how a shock generating type II bursts forms without
the occurrence of a CME eruption. Here, we aim to determine the physical
mechanism responsible for a type II burst which occurs in the absence a CME. By
using radio imaging from the Nan{\c c}ay Radioheliograph, combined with
observations from the Solar Dynamics Observatory and the Solar Terrestrial
Relations Observatory spacecraft, we investigate the origin of a type II radio
burst that appears to have no temporal association with a white-light CME. We
identify a typical type II radio burst with band-split structure that is
associated with a C-class solar flare. The type II burst source is located
above the flaring active region and ahead of disturbed coronal loops observed
in extreme ultraviolet images. The type II is also preceded by type III radio
bursts, some of which are in fact J-bursts indicating that accelerated electron
beams do not all escape along open field lines. The type II sources show
single-frequency movement towards the flaring active region. The type II is
located ahead of a faint extreme-ultraviolet (EUV) front propagating through
the corona.
