Interstellar absorption lines in the spectrum of sigma SCO using Copernicus observations

Details Interstellar absorption lines in the spectrum of sigma SCO using Copernicus observations Interstellar absorption lines in the spectrum of sigma SCO using Copernicus observations

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986inpr.conf..159a&link_type=abstract

In NASA. Ames Research Center Summer School on Interstellar Processes: Abstracts of Contributed Papers p 159-160 (SEE N87-15043

Computer Science

Absorption Spectra, Abundance, Interplanetary Dust, Line Spectra, Vapor Phases, Interstellar Chemistry, Interstellar Extinction, Oao 3, Stellar Composition

Scientific paper

Since the launch of Copernicus in 1972, studies have been made of the depletion of gas-phase elements onto dust grains. A few stars have been studied in detail, resulting in a standard depletion pattern which has since been used for comparison. Recent developments, however, have suggested that this standard pattern may need to be re-examined. Some weak, semi-forbidden lines were detected recently which may be able to resolve some of the ambiguities. Studies of single elements have shown that depletion of carbon and oxgyen are much smaller than previously determined. The high resolution ultraviolet spectral scans of sigma Sco were originally made in 1973, but have only recently been analyzed. All these stars are bright and moderately reddened. All four stars will be analyzed in detail, but sigma Sco is the first one completed. The data has broad coverage of ions, making these stars excellent candidates for determination of accurate depletions. A profile-fitting analysis was used rather than curves-of-growth in order to determine separate abundances and depletions in components separated by several km/sec.

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