Structure of Stationary Photodissociation Fronts

Abstract

The structure of stationary photodissociation fronts is revisited. H<SUB>2</SUB> self-shielding is discussed, including the effects of line overlap. We find that line overlap is important for N(H<SUB>2</SUB>) ≥ 10<SUP>20</SUP> cm<SUP>-2</SUP>, with a factor-of-2 suppression of pumping rates at column densities N(H<SUB>2</SUB>) 3 x 10<SUP>20</SUP> cm<SUP>-2</SUP> cm<SUP>-2</SUP>. We compute multiline UV pumping models and compare these with simple analytic approximations for the effects of self-shielding. <P />The overall fluorescent efficiency of the photodissociation front is obtained for different ratios of χ/n<SUB>H</SUB> (where χ characterizes the intensity of the illuminating ultraviolet radiation) and different dust extinction laws. The dust optical depth τ<SUB>pdr</SUB> to the point where 50% of the H is molecular is found to be a simple function of a dimensionless quantity φ<SUB>0</SUB> depending on χ/n<SUB>H</SUB>, the rate coefficient R(T) for H<SUB>2</SUB> formation on grains, and the UV dust opacity. The fluorescent efficiency of the photodissocation region (PDR) also depends primarily on φ for χ ≤ 3000 and n<SUB>H</SUB> ≤ 10<SUP>4</SUP> cm<SUP>-3</SUP>; for stronger radiation fields and higher densities, radiative and collisional depopulation of vibrationally excited levels interferes with the radiative cascade. We show that the emission spectrum from the PDR is essentially independent of the color temperature T<SUB>color</SUB> of the illuminating radiation for 10<SUP>4</SUP> K T<SUB>color</SUB> but shows some sensitivity to the rotation-vibration distribution of newly formed H<SUB>2</SUB>. The 1-0 S(1)/2-1 S(1) and 2-1 S(1)/6-4 Q(1) intensity ratios, the ortho/para ratio, and the rotational temperature in the v = 1 and v = 2 levels are computed as functions of the temperature and density for different values of χ/n<SUB>H</SUB>. <P />We apply our models to the reflection nebula NGC 2023. Apparent inconsistencies between published K-band and far-red spectroscopy of this object are discussed; we adjust the two sets of observations for consistency. We are able to reproduce approximately the (adjusted) observations with models having χ = 5000, n<SUB>H</SUB> = 10<SUP>5</SUP> cm<SUP>-3</SUP>, and a reasonable viewing angle. Further observations of NGC 2023 will be valuable to clarify the uncertain spatial structure of the emission.