The cooling of astrophysical media by HD

Details The cooling of astrophysical media by HD The cooling of astrophysical media by HD

Jun 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000mnras.314..753f&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 314, Issue 4, pp. 753-758.

Astronomy and Astrophysics

Astronomy

52

Molecular Data, Molecular Processes, Ism: Molecules, Cosmology: Miscellaneous

Scientific paper

The results of recent quantum mechanical calculations of cross-sections for rotational transitions within the vibrational ground state of HD are used to evaluate the rate of radiative energy loss from gas containing HD, in addition to H, He and H2. The cooling function for HD (i.e. the rate of cooling per HD molecule) is evaluated in steady state on a grid of values of the relevant parameters of the gas, namely the gas density and temperature, the atomic to molecular hydrogen abundance ratio and the ortho:para-H2 density ratio. The corresponding cooling function for H2, previously computed by Le Bourlot et al., is slightly revised to take account of transitions induced by collisions with ground-state ortho-H2 (J=1). The cooling functions and the data required for their calculation are available from http://ccp7.dur.ac.uk/. We then make a study of the rate of cooling of the primordial gas through collisions with H2 and HD molecules. In this case, radiative transitions induced by the cosmic background radiation field and, in the case of H2, collisional transitions induced by H+ ions should additionally be included.

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