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Title:
PB 6 and its central star
Authors:
Kaler, James B.; Shaw, Richard A.; Feibelman, Walter A.; Imhoff, Catherine L.
Affiliation:
AA(Illinois, University, Urbana), AB(Space Telescope Science Institute, Baltimore, MD), AC(NASA, Goddard Space Flight Center, Greenbelt, MD), AD(Computer Sciences Corp., Lanham, MD)
Publication:
Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 103, Jan. 1991, p. 67-78. (PASP Homepage)
Publication Date:
01/1991
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
O STARS, PLANETARY NEBULAE, STELLAR COMPOSITION, ULTRAVIOLET ASTRONOMY, EMISSION SPECTRA, IUE, SPECTRAL LINE WIDTH, STELLAR LUMINOSITY, STELLAR SPECTRA
DOI:
10.1086/132796
Bibliographic Code:
1991PASP..103...67K

Abstract

It is found that the hot nucleus of the Type I southern planetary nebula PB 6 is a member of the rare class of O VI stars. The blended O VI 3811 + 3834 emission doublet is one of the strongest seen, with an equivalent width (relative to the stellar continuum) of about 400 A. The helium, nitrogen, and carbon abundances are all very high for the core mass and the relations found by Kaler and Jacoby (1990). The Ne/O ratio, at 0.17, is close to the norm found for planetaries, which supports the high O/H, while the S/O is roughly solar.

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