Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1974
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974a%26a....37..305d&link_type=abstract
Astronomy and Astrophysics, vol. 37, no. 2, Dec. 1974, p. 305-311.
Astronomy and Astrophysics
Astronomy
51
Carbon, Fine Structure, Interstellar Matter, Line Spectra, Nebulae, Error Analysis, Gas Density, Ground State, Interstellar Extinction, Oao 3, Spaceborne Astronomy, Spectral Line Width, Transition Probabilities, Ultraviolet Spectra
Scientific paper
With two f-values of C I lines obtained from the spectra of zeta Pup and gamma(2) Vel, it is shown that the interstellar C I spectrum in zeta Oph obeys an optical-depth relation similar to that for Na I, and the relative strengths of 19 multiplets are determined from this relation. The dominant processes which excite neutral carbon are used to calculate populations of the fine-structure levels as functions of the density of H nuclei and the temperature, and evidence is found that the C I lines are formed in the dense cloud in front of zeta Oph at a heliocentric velocity of -14.4 km/s. It is noted that the observed column-density ratios of the neutral carbon fine-structure levels lead to a total H nuclei density of about 220 to 660 per cu cm, while the electron density and observed C(+) abundance indicate a value of 10,000 per cu cm, with a 0.05 pc thick gas layer.
de Boer Klaas. S.
Morton Donald C.
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