On the interpretation of Copernicus observations of interstellar absorption lines in front of XI Persei

Details On the interpretation of Copernicus observations of interstellar absorption lines in front of XI Persei On the interpretation of Copernicus observations of interstellar absorption lines in front of XI Persei

Jan 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975a%26a....38...29g&link_type=abstract

Astronomy and Astrophysics, vol. 38, no. 1, Jan. 1975, p. 29-39.

Astronomy and Astrophysics

Astronomy

37

Absorption Spectra, Interstellar Extinction, Spaceborne Astronomy, Spectral Line Width, Stellar Spectra, Ultraviolet Absorption, Abundance, Astronomical Models, Far Ultraviolet Radiation, Line Spectra, Oao 3, Td-1 Satellite, Ultraviolet Spectra

Scientific paper

Observations of the equivalent widths of UV interstellar absorption lines in the spectrum of Xi Per are analyzed using models of the velocity distribution of interstellar matter in front of the star, derived from known profiles of optical interstellar lines. It is shown that except for atoms like C, Mg, S, Na, and K, observations can be explained only if both clouds and a high-velocity dispersion gas containing 4 to 35 percent of a particular element are present in the interstellar medium. Limits are set on the column densities of the different atoms and ions in front of Xi Per by a curve-of-growth analysis using models of interstellar gas in which high-velocity dispersion material is added to the basic clouds. The results indicate that Na, K, S, and Ar are probably not much depleted in the interstellar gas, while Mg, Si, P, Ca, and Ti are depleted to various degrees. Some quantitative data on the degree of ionization in the high-velocity dispersion medium are presented, and the degree of ionization in the clouds is calculated.

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