Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984nascp2349..361a&link_type=abstract
In NASA. Goddard Space Flight Center Future of Ultraviolet Astronomy Based on Six Years of IUE Res. p 361-364 (SEE N85-20961 1
Astronomy and Astrophysics
Astronomy
6
Auriga Constellation, Eclipsing Binary Stars, Hot Stars, Light Curve, Stellar Spectrophotometry, Ultraviolet Spectra, Emission Spectra, F Stars, Interstellar Matter, Primary Cosmic Rays, Secondary Cosmic Rays, Stellar Occultation, Stellar Radiation, Ultraviolet Astronomy
Scientific paper
The major characteristics in the UV of the 1982 to 84 eclipse of Zeta Aur, from first through third contact are summarized. From 1500 to 3200 A, the spectrum is dominated by periodic changes in continuum levels, apparently due to Cepheid-like pulsation of the primary, superimposed upon the decrease in light due to the eclipse itself. No large increase in the 2200 A dip is found, so that if the cool disk is comprised of cool dust grains, they must be larger than typical interstellar grains. Comparison with other A-F supergiants are inconclusive whether a hot companion is seen, although excess UV flux is present shortward of 1400 A. The only strong emission lines in the UV are 0 I 1304 and Mg II 2800. The O I is present outside of eclipse and shows variations of a factor of two during totality. The absence of strong eclipse effects on it leaves some doubt as to whether it arises from the F-type primary, the secondary, or intrasystem gas. The Mg II emission, which was unveiled as the F-star continuum decreased on ingress, developed a broad, blue-shifted component of -300 k/s, which is speculated that it may be a signature of accretion by the secondary of gas ejected by the primary.
Ake Thomas B. III
Simon Theodore
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