MAGNETIC FIELD STRENGTHS IN PHOTODISSOCIATION REGIONS

We measure carbon radio recombination line (RRL) emission at 5.3 GHz ?> toward four H ii regions with the Green Bank Telescope to determine the magnetic field strength in the photodissociation region (PDR) that surrounds the ionized gas. Roshi suggests that the non-thermal line widths of carbon RRLs from PDRs are predominantly due to magneto-hydrodynamic waves, thus allowing the magnetic field strength to be derived. We model the PDR with a simple geometry and perform the non-LTE radiative transfer of the carbon RRL emission to solve for the PDR physical properties. Using the PDR mass density from these models and the carbon RRL non-thermal line width we estimate total magnetic field strengths of B ∼ 100 – 300 ?> &mgr; G ?> in W3 and NGC 6334A. Our results for W49 and NGC 6334D are less well constrained with total magnetic field strengths between B ∼ 200 – 1000 ?> &mgr; G ?> . H i and OH Zeeman measurements of the line of sight magnetic field strength ( B los ?> ), taken from the literature, are between a factor of ∼ 0.5 – 1 ?> of the lower bound of our carbon RRL magnetic field strength estimates. Since ∣ B los ∣ ≤ B ?> , our results are consistent with the magnetic origin of the non-thermal component of carbon RRL widths.