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Implicit and explicit raytracing-photoionisation algorithms have beenimplemented in the author's radiation-magnetohydrodynamics code. The algorithmsare described briefly and their efficiency and parallel scaling areinvestigated. The implicit algorithm is more efficient for calculations whereionisation fronts have very supersonic velocities, and the explicit algorithmis favoured in the opposite limit because of its better parallel scaling. Theimplicit method is used to investigate the effects of initially uniformmagnetic fields on the formation and evolution of dense pillars and cometaryglobules at the boundaries of HII regions. It is shown that for weak and mediumfield strengths an initially perpendicular field is swept into alignment withthe pillar during its dynamical evolution, matching magnetic field observationsof the`Pillars of Creation' in M16. A strong perpendicular magnetic fieldremains in its initial configuration and also confines the photoevaporationflow into a bar-shaped, dense, ionised ribbon which partially shields theionisation front.

Radiation-MHD simulations of pillars and globules in HII regions