The variation of interstellar element abundances with hydrogen density

Details The variation of interstellar element abundances with hydrogen density The variation of interstellar element abundances with hydrogen density

Sep 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.222..143k&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 222, Sept. 1, 1986, p. 143-147. SERC-supported research

Astronomy and Astrophysics

Astronomy

5

Abundance, Astronomical Models, Gas Density, Hydrogen Clouds, Interstellar Gas, Spatial Distribution, Gas Temperature, Least Squares Method

Scientific paper

The variation of the interstellar nitrogen, oxygen and magnesium abundances with mean line-of-sight density >nH< is analysed in terms of a two-component model first employed by Jenkins, Savage and Spitzer (1986), which consists of warm, low-density neutral gas and cold clouds. In all cases the gas-phase abundances have been deduced using reliable oscillator strengths specifically calculated for this purpose. Depletions in the warm and cold gas, denoted Dw and Dc respectively, are derived from non-linear least-squares fits to the data. Values of Dw for the species considered are found to be small (≅0.1 dex), consistent with the low reddening and hence grain content in such sight-lines.

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