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Chemical enrichment in the early Galaxy

Published online by Cambridge University Press:  01 June 2008

Torgny Karlsson
Torgny Karlsson*
Affiliation:
NORDITA, AlbaNova University Center, SE-106 91, Stockholm, Sweden School of Physics, The University of Sydney, 2006 NSW, Australia email: torgny@physics.usyd.edu.au
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Abstract

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The chemical enrichment by the first sources of light in the universe ultimately set the stage for the subsequent evolution of the Milky Way system. The oldest and, usually, the most-metal poor stars are our ‘near-field’ link to this ancient epoch as they, apart from tracing the chemical enrichment itself, also indirectly hold information on, e.g., the conditions for star formation and feed-back effects in the early universe. In particular, I will discuss the possible origins of the relatively large number of carbon enhanced metal-poor stars in the Galactic halo. Furthermore, I will argue that the apparent absence of the chemical signature of so-called pair-instability supernovae (PISNe), which are a natural consequence of current theoretical models for primordial star formation at the highest masses, may arise from a subtle observational selection effect. Whereas most surveys traditionally focus on the most metal-poor stars, early PISN enrichment is predicted to ‘overshoot’, reaching enrichment levels of [Ca/H] ~ −2.5 that would be missed by current searches.

Keywords

stars: abundancesstars: formationstars: Population IIGalaxy: evolutionGalaxy: formationGalaxy: halo
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S254: The Galaxy Disk in Cosmological Context , June 2008 , pp. 343 - 348
Copyright
Copyright © International Astronomical Union 2009

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