  We have carried out an in-depth study of three bright-rimmed clouds SFO 11,
SFO 11NE and SFO 11E associated with the HII region IC 1848, using observations
carried out at the James Clerk Maxwell Telescope (JCMT) and the Nordic Optical
Telescope (NOT), plus archival data from IRAS, 2MASS and the NVSS. We show that
the overall morphology of the clouds is reasonably consistent with that of
radiative-driven implosion (RDI) models developed to predict the evolution of
cometary globules. There is evidence for a photoevaporated flow from the
surface of each cloud and, based upon the morphology and pressure balance of
the clouds, it is possible that D-critical ionisation fronts are propagating
into the molecular gas. The primary O star responsible for ionising the
surfaces of the clouds is the 06V star HD17505. Each cloud is associated with
either recent or ongoing star formation: we have detected 8 sub-mm cores which
possess the hallmarks of protostellar cores and identify YSO candidates from
2MASS data. We infer the past and future evolution of the clouds and
demonstrate via a simple pressure-based argument that the UV illumination may
have induced the collapse of the dense molecular cores found at the head of SFO
11 and SFO 11E.
