An Abundance Analysis of the Primary Star of the Peculiar Eclipsing Binary ɛ Aurigae out of the Eclipsing Phase

Details An Abundance Analysis of the Primary Star of the Peculiar Eclipsing Binary ɛ Aurigae out of the Eclipsing Phase An Abundance Analysis of the Primary Star of the Peculiar Eclipsing Binary ɛ Aurigae out of the Eclipsing Phase

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010pasj...62.1381s&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.62, No.6, pp.1381--1390

Astronomy and Astrophysics

Astronomy

3

Stars: Abundances, Stars: Eclipsing Binaries, Stars: Individual (Ɛ Aurigae), Stars: Spectroscopy

Scientific paper

A detailed abundance analysis of the primary star of ɛ Aur before an eclipse was carried out using a very high signal-to-noise ratio optical-region spectrum. An A7 Iab supergiant HD 81471, presumably a member of the Vela OB1 association, was used as a reference. We obtained atmospheric parameters (Teff, log g, and ξt) to be (8025 K, 1.0 and 10 km s-1) and (8050 K, 1.0 and 7 km s-1) for ɛ Aur and HD 81471, respectively. The abundances of Mg, Si, S, Ca, Sc, Ti, Cr, and Fe were very close to the solar abundances in both stars. Light elements C and O were under-abundant, while N and Na were over-abundant in both stars, after correcting for non-LTE effects. Definite under-abundances of Sr were detected in both stars. Slight, but definite, over-abundances were found in ɛ Aur for the s-process elements Y, Zr, and Ba, when compared with the results of HD 81471. Enhancements in the abundances of N, Na, and s-process elements might indicate the occurences of thermal dredge-up and the s-process nucleosynthesis in ɛ Aur during the past evolution.

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