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Full Description
The open cluster NGC 6791 is now considered both the oldest and the most metal-rich known. Its age is 8 -10 Gyrs, twice as old as the canonical solar-metallicity cluster M67 (Garnavich et al. 1994; Demarque, Green, & Guenther 1992; Tripicco et al. 1995). That its metallicity is significantly above solar is suggested from moderate-resolution spectroscopy and from a mismatch of its color-magnitude diagram (CMD) with solar-metallicity isochrones. Tripicco et al. (1995) find [Fe/H] = +0.27 to +0.44. The cluster population is rich. In addition to about a dozen red giants and two dozen red horizontal-branch stars, the cluster has several very hot HB stars (Kaluzny & Udalski 1992). Liebert et al. (1994) have shown that the extremely blue stars are mostly sdB/sdO stars and at least 3 or 4 are likely cluster members, the first ever discovered in an open cluster. These may provide the key to the puzzling upturn in ultraviolet flux below 1500A seen in many high-metallicity systems (Burstein et al. 1988; Ferguson et al. & Liebert 1993).
Contents
Conference Papers in order of Presentation.- Big Bang Nucleosynthesis.- Light Elements Abundances: New Insights on Stellar Mixing and Galactic Production.- The First Stars.- Type 1A Supernovae and Chemical Evolution of Galaxies.- The Chemical Evolution of Light Elements in Our Galaxy.- Nucleosynthesis in Red Giant Stars.- Fluorine Production from AGB and WR Stars.- Deuterium Abundance in the Local ISM.- Abundances in Halo Population Stars.- Abundances in the Galactic Disk.- Abundances in a Hot Horizontal-Branch Star in the Old Open Cluster NGC/6791.- On the Progenitors of Type Ia Supernovae.- Abundances from z = 0 to z = 5.- Enrichment of Heavy Elements in Clusters of Galaxies.- On the Origin of Metallicity in Lyman-Alpha Forest Systems.- A Metal Enriched Dark Cluster of Galaxies at Z = 1.- Are Elliptical Galaxies Really Metal-Rich?.- Chemical Evolution of Spiral Galaxies from Redshift 4 to the Present.- Age Problem Based on the Abundance Ratio from a High-Redshift QSO.- Stellar Yields and Chemical Evolution.- The Formation of First Generation Stars and Globular Clusters in Protogalactic Clouds.- Constraints on Galaxy Formation from Extragalactic Globular Clusters.- The Evolution of Old Stellar Populations in Our Galaxy.- Chemical Evolution of the Magellanic Clouds.- Global Evolution of the Stars, Gas, Metals, and Dust in Galaxies.- Conference Summary.- Conference Abstracts in Alphabetical Order.- Nitrogen Abundance in Oxygen-Rich Giants through K to late M.- Asymmetrical Delayed Detonation From a 3D Hydrosimulation of a White Dwarf Explosion.- Numerical Simulations of the Chemical Evolution of Galaxies Using Treecode-SPH.- Chemical Evolution of Damped Lyman ? Systems.- Abundances in Metal-Rich Stars.- Abundance Pattern of Supergiants in the Field of the SmallMagellanic Cloud and in the Cluster NGC 330.- Age and Metallicity Distribution of the Disk Stars from Edge-on Galaxies.- Evolution of the Colour-Magnitude Relation of Elliptical Galaxies.- The Optical Properties of Carbon and Graphite depend on Crystal Structure and Temperature.- Improved Theoretical Stellar Library for Population Synthesis Models.- Chemical and Spectrophotometric Evolution of Optically Identified QSO Absorption Systems.- Comparison of Nucleosynthesis Models.- The Galactic Disc Age-Metallicity Relation.- Analysis of Elemental Carbon and Oxygen Abundances in Carbon Stars — They have turned out to be more Carbon-Rich than believed.- Abundances in Evolved Intermediate Mass Stars.- Spectral Energy Distributions of z > 2 Galaxies in the Hubble Deep Field.- Blue 'Elliptical' Galaxies in the Hubble Deep Field.- The Symbiotic-Barium Stars Link.- The Spectral Evolution of Elliptical Galaxies in FIR and beyond.- Nucleosynthesis in ONEMG Novae: Comparison with Observations.- Constraints on Cosmic Chemical Evolution from the Gamma-Ray Background.- Disk-Wind Models for Broad Absorption Line QSO's.- Supernova Observing Web (SNOW) Project with the Public Astronomical Observatories in Japan.- Element Abundances in Metal-Poor Stars.
