Molecule formation in quasar broad-line cloud gas

Details Molecule formation in quasar broad-line cloud gas Molecule formation in quasar broad-line cloud gas

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...321..907k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 321, Oct. 15, 1987, p. 907-911.

Statistics

Computation

9

Emission Spectra, Galactic Nuclei, Interstellar Gas, Line Spectra, Molecular Clouds, Quasars, Abundance, Computational Astrophysics, Gas Pressure, Light Speed, Lyman Beta Radiation, X Ray Spectra

Scientific paper

Models for the broad-line emitting clouds of quasars typically assume that the clouds have column densities of at most 10 to the 23rd/sq cm. The consequences of relaxing this assumption are examined, and it is shown that: (1) at slightly larger column densities the gas may cool to about 1000 K as a result of molecule formation; (2) in much of the molecule-forming region the temperature may have either of two values, about 1000 K or 6000-8000 K; (3) the strengths of most observable optical lines, including C II semiforbidden 2326-A lines and Fe II lines, are unaffected by such large column densities; and (4) lines from low-ionization species such as Na I are readily formed at large column densities. Observations of such lines provide evidence for large cloud column densities.

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