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Bright-rimmed clouds (BRCs) are formed at the periphery of H$~$II regions asthe radiation from the central star interacts with dense gas. The ionizationand resulting compression of the clouds may lead to cloud disruption causingsecondary star formation depending on the stellar and gas parameters. Here weuse R-band polarimetry to probe the plane-of-the sky magnetic field in the twonear-by BRCs IC\,59 and IC\,63. Both nebulae are illuminated by $\gamma$ Caswith the direction of ionizing radiation being orientated parallel orperpendicular to the local magnetic field, allowing us to probe the importanceof magnetic field pressure in the evolution of BRCs. Because of the proximityof the system ($\sim$200pc) we have acquired a substantial sample of over 500polarization measurements for stars background to the nebulae. On large scales,the magnetic field geometries of both clouds are anchored to the ambientmagnetic field. For IC 63, the magnetic field is aligned parallel to thehead-tail morphology of the main condensation, with convex morphology relativeto the direction of the ionizing radiation. We estimate the plane of the skymagnetic field strength in IC\,63 to be $\sim90\mu$G. In IC\,59, the projectedmagnetic field follows the M shape morphology of the cloud. Here, field linespresent a concave shape with respect to the direction of the ionizing radiationfrom $\gamma$ Cas. Comparing our observations to published theoretical modelswe find good general agreement, supporting the importance of magnetic fields inBRC evolution.

Magnetic field structure of IC 63 and IC 59 associated to H II region - Sh 185