SIMBAD references

Far-ultraviolet (FUV) photons expel electrons from interstellar dust grains and the excess kinetic energy of the electrons is converted into gas thermal energy through collisions. This photoelectric heating is believed to be the main heating mechanism in cool H I clouds. The heating rate cannot be directly measured, but it can be estimated through observations of the [C II] line emission, since this is believed to be the main coolant in regions where the photoelectric effect dominates the heating. Furthermore, the comparison of the [C II] emission with the far-infrared (FIR) emission allows us to constrain the efficiency of the photoelectric heating using model calculations that take into account the strength of the radiation field. Recent [C II] observations carried out with the Infrared Space Observatory satellite have made this study possible.

In this work, we study the correlation between FUV absorption and FIR emission using three-dimensional models of the density distribution in H I clouds. The density distributions are obtained as the result of numerical simulations of compressible magnetohydrodynamic turbulence, with rms sonic Mach numbers of the flow ranging from subsonic to highly supersonic, 0.6≤M_S≤10. The FIR intensities are solved with detailed radiative transfer calculations. The [C II] line radiation is estimated assuming local thermodynamic equilibrium where the [C II] line cooling equals the FUV absorption multiplied by the unknown efficiency of the photoelectric heating, ε.

The average ratio between the predicted [C II] and FIR emissions is found to be remarkably constant between different models, implying that the derived values of ε should not depend on the rms Mach number of the turbulence. The comparison of the models with the empirical data from translucent, high-latitude clouds yields an estimate of the photoelectric heating efficiency of ε∼2.9x10^–2 on the basis of the dust model of Li & Draine. This value confirms previous theoretical predictions.

The observed correlation between [C II] and FIR emission contains a large scatter, even within individual clouds. Our models show that most of the scatter can be understood as resulting from the highly fragmented density field in turbulent H I clouds. The scatter can be reproduced with density distributions from supersonic turbulence, while subsonic turbulence fails to generate the observed scatter.