Thermal and Chemical Evolution of Interstellar Clouds

Details Thermal and Chemical Evolution of Interstellar Clouds Thermal and Chemical Evolution of Interstellar Clouds

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.247..500f&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 247, NO. 3/DEC1, P. 500, 1990

Astronomy and Astrophysics

Astronomy

15

Scientific paper

We have studied the thermal and chemical evolution of interstellar clouds from an initially atomic to a finally molecular gas, in equilibrium. The process of H2 formation on grain surfaces leads to the production of heavier molecules, such as CO, from atoms and ions, such as C and C+. At the same time, kinetic energy is released into the gas, resulting in a secondary temperature maximum which can attain T ≍ 100 K and last several million years, enhancing the emission lines of C I, C II and CO. The temporal evolution of the ratio of population densities H2(j=1):H2(j=0) is also computed.

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