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Abundances in a Hot Horizontal-Branch Star in the Old Open Cluster NGC/6791

Published online by Cambridge University Press:  19 July 2016

R.C. Peterson  and
E.M. Green
R.C. Peterson
Affiliation:
Astrophysical Advances, Palo Alto, CA UCO/Lick Observatories, Santa Cruz, CA
E.M. Green
Affiliation:
Steward Observatory, University of Arizona, Tucson, AZ

Abstract

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The open cluster NGC 6791 is more metal-rich than any other open cluster, yet several hot blue horizontal branch (BHB) stars are probable members. We have performed an abundance analysis of the coolest such star, 2-17, which has a radial velocity and a proper motion which support cluster membership. We find parameters typical of a metal-rich BHB star, with rotational velocity = 16 ± 1 km/s, an effective temperature Teff = 7250 ± 150 K, log gravity = 3.5 ±0.5 dex, and an iron abundance more than twice solar, [Fe/H] = +0.4 ± 0.1 dex. The light even-Z elements Mg, Ca, and Si are further enhanced, ruling out A-star peculiarities. Its analysis thus establishes the cluster metallicity accurately, free from serious blending which is problematical in metal-rich giants. Abundances of C, N, and O suggest little mixing. Visual comparison of the spectra of red HB stars in the cluster with that of the field star μ Leo indicates that the spectra are indistinguishable except for stronger CN in the former.

The high iron abundance, the light-element overabundances, the spectral similarity to strong-lined field giants, and the extensive presence of hot stars all highlight the fact that this old open cluster provides an excellent template for the study of metal-rich extragalactic systems. Properties of cluster members should establish not only accurate abundances for comparison with scenarios of nucelosynthesis and star formation, but also provide a testbed for ideas of the production of hot stars in a metal-rich environment, and so for the generation of the ultraviolet upturn in elliptical galaxies.

Type
Conference Papers in order of Presentation
Information
Symposium - International Astronomical Union , Volume 187: Cosmic Chemical Evolution , 2002 , pp. 97 - 102
Copyright
Copyright © 2002 

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