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Copernicus studies of interstellar material in the Perseus II complex. III - The line of sight to Zeta PerseiUltraviolet spectrophotometric data obtained with Copernicus are used to analyze the distribution, composition, density, temperature, and kinematics of the interstellar material along the line of sight to Zeta Persei. The far-UV extinction curve for the star is evaluated along with the kinematics of the interstellar gas, observations of atomic and molecular hydrogen, curves of growth for neutral and ionized species, atomic abundances and depletions, ionization equilibria, and observations of CO and OH lines. The results show that there are apparently three clouds along the line of sight to Zeta Persei: a main cloud at approximately +13 km/s which contains most of the material and forms all the neutral and molecular lines as well as most of the ionic lines, a second component at +22 km/s which must contribute to the strong UV lines of most ions, and a third component at roughly +2 km/s which gives rise to a strong Si III line at 1206 A. It is also found that the UV extinction curve has a somewhat steep far-UV rise, indicating the presence of a substantial number of small grains, and that about 30% of the hydrogen nuclei over the entire line of sight are in molecular form.
Document ID
19780030791
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Snow, T. P., Jr.
(Princeton University New Observatory, Princeton, N.J., United States)
Date Acquired
August 9, 2013
Publication Date
September 15, 1977
Publication Information
Publication: Astrophysical Journal
Subject Category
Astrophysics
Accession Number
78A14700
Funding Number(s)
CONTRACT_GRANT: NAS5-23576
Distribution Limits
Public
Copyright
Other

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