Download Chemical Evolution from Zero to High Redshift: Proceedings by Bengt Gustafsson (auth.), Jeremy R. Walsh, Michael R. Rosa PDF

By Bengt Gustafsson (auth.), Jeremy R. Walsh, Michael R. Rosa (eds.)

The observational and interpretive instruments for the research of chemical evolution are transforming into mature adequate that they are often utilized with a few self assurance to extra-galactic structures and built-in populations at more and more excessive redshift. This publication is dedicated to the learn of the interaction among varied tools of measuring chemical abundances with astrophysical versions. reviews of chemical abundances and evolution from stars, inter-stellar medium and native workforce galaxies at 0 redshift to far-off galaxies, clusters of galaxies and inter-galactic medium at excessive redshift are awarded. There also are synopses on growth in instrumentation for abundance determination.

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Extra info for Chemical Evolution from Zero to High Redshift: Proceedings of the ESO Workshop Held at Garching, Germany, 14–16 October 1998

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15 dex smaller than those for the Sun , implying the weil known result that t he Sun is heavy eleme nt rieh for its age . The GIO values for Orion , M8, and M17 are higher t ha n in the Sun . T hese differences mig ht be due to Galactic chemical evolution . Galactic H II Region Abundan ces 37 T hc best galactic I-I II region to determine the He ab undance is M17. 0 values from this neb ula shou ld be used as strong observational constraints to test mode ls of Ga lactic chemical evolution. lt is a pleasure to acknow ledge many fruitful discussions wit h Leticia Carigi, Cesar Esteban, Miriam Pefia, and Silvia Torres-Peimbcrt.

E. through o-processing in massive stars, and returned to the ISM through SN Type 11 explosions. Henee it is encouraging to eonfirm that their variations through the Galactic disk are weil eorrelated . 3 Probing the Inner Regions of the Galaetic Disk Metallieity variations in the inner regions of the Galactie disk have until reeently been mainly ignored due to the difficulty in optieally probing these high extinction regions. Determinations have relied on infra-red observations of nebular regions, but from such spectra the element range provided is limited (AfHerbach et al.

1985 , Ap . 1 . 295, 604 Thielemann, F. , Nom oto, K. , Hashimoto , M. 1996 , Ap, J . -K . et al. 1998, in N uclear and Particle Astrophysics, eds. 1 . Hirsch , D. P age, Ca mbri dge Univ . Press, p . , Bender , R. 1998 , MNRAS 296 , 119 Weav er , T. A. E. 1993 , Phys. Rep . C . et a!. 1995 , Phys. E. et a!. 1997, Nucl. Phys. A. 1994, Ap . E. A . 1995, Ap, J. Supp!. 101, 181 Woosley, S. E . et a!. 1994, Ap . 1. 433, 229 Abundance Gradients from Massive, Early-Type Stars - the Milky Way and Beyond Stephen J.

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