Modeling of diffuse molecular gas applied to HD 102065 observations

Aims. We model a diffuse molecular cloud present along the line of sight to the star HD 102065. We compare our modeling with observations to test our understanding of physical conditions and chemistry in diffuse molecular clouds. Methods. We analyze an extensive set of spectroscopic observations which characterize the diffuse molecular cloud observed toward HD 102065. Absorption observations provide the extinction curve, H(2), C I, CO, CH, and CH(+) column densities and excitation. These data are complemented by observations of C(+), CO and dust emission. Physical conditions are determined using the Meudon PDR model of UV illuminated gas. Results. We find that all observational results, except column densities of CH, CH(+) and H(2) in its excited (J >= 2) levels, are consistent with a cloud model implying a Galactic radiation field (G similar to 0.4 in Draine's unit), a density of 80 cm(-3) and a temperature (60-80 K) set by the equilibrium between heating and cooling processes. To account for excited (J >= 2) H(2) levels column densities, an additional component of warm (similar to 250 K) and dense (n(H) >= 104 cm(-3)) gas within 0.03 pc of the star would be required. This solution reproduces the observations only if the ortho-to-para H(2) ratio at formation is similar to 1. In view of the extreme physical conditions and the unsupported requirement on the ortho-to-para ratio, we conclude that H(2) excitation is most likely to be accounted for by the presence of warm molecular gas within the diffuse cloud heated by the local dissipation of turbulent kinetic energy. This warm H(2) is required to account for the CH(+) column density. It could also contribute to the CH abundance and explain the inhomogeneity of the CO abundance indicated by the comparison of absorption and emission spectra.