Magnetic field structure of IC 63 and IC 59 associated to H II region -
  Sh 185
  Bright-rimmed clouds (BRCs) are formed at the periphery of H$~$II regions as
the radiation from the central star interacts with dense gas. The ionization
and resulting compression of the clouds may lead to cloud disruption causing
secondary star formation depending on the stellar and gas parameters. Here we
use R-band polarimetry to probe the plane-of-the sky magnetic field in the two
near-by BRCs IC\,59 and IC\,63. Both nebulae are illuminated by $\gamma$ Cas
with the direction of ionizing radiation being orientated parallel or
perpendicular to the local magnetic field, allowing us to probe the importance
of magnetic field pressure in the evolution of BRCs. Because of the proximity
of the system ($\sim$200pc) we have acquired a substantial sample of over 500
polarization measurements for stars background to the nebulae. On large scales,
the magnetic field geometries of both clouds are anchored to the ambient
magnetic field. For IC 63, the magnetic field is aligned parallel to the
head-tail morphology of the main condensation, with convex morphology relative
to the direction of the ionizing radiation. We estimate the plane of the sky
magnetic field strength in IC\,63 to be $\sim90\mu$G. In IC\,59, the projected
magnetic field follows the M shape morphology of the cloud. Here, field lines
present a concave shape with respect to the direction of the ionizing radiation
from $\gamma$ Cas. Comparing our observations to published theoretical models
we find good general agreement, supporting the importance of magnetic fields in
BRC evolution.
