Abstract
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.
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