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

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

The observational and interpretive instruments for the learn of chemical evolution are becoming mature adequate that they are often utilized with a few self belief to extra-galactic structures and built-in populations at more and more excessive redshift. This e-book is dedicated to the research of the interaction among diverse tools of measuring chemical abundances with astrophysical types. experiences of chemical abundances and evolution from stars, inter-stellar medium and native team galaxies at 0 redshift to far away galaxies, clusters of galaxies and inter-galactic medium at excessive redshift are provided. There also are synopses on development in instrumentation for abundance determination.

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Extra resources 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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25. For He, Ne, Ar, N, S, and CI they estimate that th e du st correction is negligibl e. Also in Table 2 th e Orion ncbul a a bu ndances a re corn pa rcd with t he so lar ones. Fro m t his compari son it follows t hat, with t hc cxce pt ion of C a nd Fe, t he heavy eleme nts are overa bundant in t he Su n by about 0. 15 dcx, Galactic H II Region Abundances 33 Table 1. 037 Gaseous abundances given in 12 + log N(X)/ N(H), for references see text b Simpson et al. (1998) a Table 2. 02 a Abundances given in 12 + log N(X)/ N (H) bEsteban et al.

1994, Ap . 1. 433, 229 Abundance Gradients from Massive, Early-Type Stars - the Milky Way and Beyond Stephen J. Smart t Isaac Newt on Group of Telescopes, Apartado de Correos 368 , Santa Cruz de La Pairn a , 38700 , Can ary Islands, Spai n Abstract. I will presen t resul ts on a bundance gradien ts in t he Gala ctic disk as derived from det ailed sp ect ral ana lyses of hot rnain-sequ ence B-type stars. 2 dex, and I will discuss the feasibility of using more lumi nous sup ergiant stars (of similar spectral type) to estimate abundances throughout the Local Group.

G. see Rolleston ct al. 1996). More massive O-type main-sequenee stars (of typieally M. > 20M(o) ) evolve ac ross the HR-diagram through the B-type supergiant region . At th is stage in t heir lives they have luminosities of up to 106L 8 and an absolute visual magnitude dependent on th eir effective t em pera t ures, but ty piea lly M, '" -6 . A later, but similar evolutionary stage puts them in t he AF-supergiant region , Abundance Gradients from Early-Type Stars 25 where the optical flux inereases although the overallluminosity remains approximately eonstant.

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