Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993phdt........10s&link_type=abstract
Ph.D. Thesis Wisconsin Univ., Madison, WI.
Astronomy and Astrophysics
Astronomy
Absorption Spectra, Cosmic Dust, Interstellar Gas, Interstellar Matter, Line Spectra, Ultraviolet Astronomy, Abundance, Astronomical Spectroscopy, B Stars, High Resolution, Hubble Space Telescope, Silicates
Scientific paper
The emphasis of this thesis is on the gas and dust in the diffuse neutral interstellar medium. This study was conducted in two parts each of which makes use of 3.5 km s-1 resolution spectroscopic data obtained with the Goddard High Resolution Spectrograph aboard the Hubble Space Telescope. The first chapter is a detailed analysis of the gas and dust properties of the neutral absorbing regions in a single line of sight, that toward the star mu Columbae. The second chapter combines information toward multiple lines of sight in order to study the global properties of interstellar dust in the diffuse interstellar medium. Chapter one analyzes four distinct absorbing regions toward the star mu Col through absorption line data for the dominant neutral cloud species CII, OI, MgII, AlII, SiII, SII, CrII, MnII, FeII, NiII, and Zn I, as well as the nondominant species MgI, and SiIII. Column densities for these ions were determined with a typical uncertainty of plus or minus 0.1 dex. The total destruction of silicate grains in one of the absorbing regions implies which may have been disrupted by a shock with a velocity 50 is less than or equal to v is less than or equal to 200 km s-1. The main absorbing component has an element-to-element depletion pattern very similar to that of a diffuse cloud toward zeta Oph. Chapter two explores the characteristics of dust in the neutral diffuse interstellar medium which has not experienced any grain core destruction. Column densities for the abundant elements C, N, O, Mg, Si, Fe and S are taken from the literature for eight absorbing regions in the sightlines toward mu Col, zeta Oph, xi Per, HD167756, and HD93521. Depletions and dust-phase abundances which are derived for the absorbing regions suggest that Mg and Fe bearing oxides and/or metallic Fe grains are important constituents of the grain core population. Differences in the implied dust abundance based on solar and B star reference abundances are examined.
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