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Several indirect evidences indicate a magnetic origin for the non-thermalwidth of spectral lines observed toward molecular clouds. In this letter, Isuggest that the origin of the non-thermal width of carbon recombination lines(CRLs) observed from photo-dissociation regions (PDRs) near ultra-compact \HII\regions is magnetic and that the magnitude of the line width is an estimate ofthe \alfven speed. The magnetic field strengths estimated based on thissuggestion compare well with those measured toward molecular clouds withdensities similar to PDR densities. I conclude that multi-frequency CRLobservations have the potential to form a new tool to determine the fieldstrength near star forming regions.Comment: To appear in ApJ Letter

Magnetic Fields at the Periphery of Ultracompact H ii Regions from Carbon Recombination Line Observations