Chemical signatures of the intermittency of turbulence in low density interstellar clouds.

Details Chemical signatures of the intermittency of turbulence in low density interstellar clouds. Chemical signatures of the intermittency of turbulence in low density interstellar clouds.

Aug 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...300..870f&link_type=abstract

Astronomy and Astrophysics, v.300, p.870

Astronomy and Astrophysics

Astrophysics

61

Molecular Processes, Turbulence, Ism: General, Ism: Clouds, Ism: Kinematics And Dynamics, Ism: Molecules

Scientific paper

The space-time intermittent distribution of the dissipation rate of kinetic energy in turbulent interstellar clouds generates transient and localized hot regions embedded in cooler gas. The gas kinetic temperatures reached in low-density clouds, such as H I clouds, are locally large enough to overcome many activation barriers of gas phase chemical reactions and significantly increase the endothermic reaction rates. Small regions with a chemistry characteristic of hot gas are therefore expected to be found, immersed in the interiors of cold atomic clouds. We show that the estimated lifetime of the transiently hot regions is long enough for these specific signatures to develop, locally increasing the molecular abundances of OH, H_2_O, CH^+^ and HCO^+^ by several orders of magnitude above those characteristic of the surrounding gas. The column densities of species such as CH^+^ and HCO^+^ across a low-density, mostly atomic, cloud in an active stage of turbulence dissipation are shown to be comparable to observed values without any fine tuning of parameters.

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