The carbon abundance in diffuse interstellar clouds

Details The carbon abundance in diffuse interstellar clouds The carbon abundance in diffuse interstellar clouds

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...246l.147l&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 246, June 15, 1981, p. L147-L150.

Astronomy and Astrophysics

Astrophysics

15

Abundance, Carbon, Interstellar Gas, Molecular Clouds, Astrophysics, Hydrogen Clouds

Scientific paper

Liszt (1979) had argued that the depletion of carbon toward Zeta Oph had been overestimated as a result of the presence of a very narrow absorbing cloud containing the majority of the neutral species. It is shown that the total carbon column densities inferred from C I measurements generally represent a solar fraction of the H2 column density, consistent with the very small degree of depletion inferred from C I when the H2 column density is negligible. For stars with measured C II column densities, the ratio of the C II column density and the H I column density is also consistent with a solar carbon abundance and with the general segregation of the pairs C I = H2 and C II = H I whenever the abundance of molecular hydrogen is significant. An analysis shows that carbon is strongly depleted neither in denser molecular gas nor in the more tenuous atomic regions accessible to UV absorption measurements.

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