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Other [alpha] metals will have been produced in core collapse supernovae.<ref> |
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The '''Metallicity distribution function''' is an important concept in [[stellar evolution|stellar]] and [[galactic evolution]].
It is a curve of what proportion of stars have a particular [[metallicity]] ([Fe/H], the relative abundance of iron and hydrogen) of a population of stars such as in a cluster or galaxy.<ref name=Fenner2003>[http://www.publish.csiro.au/?act=view_file&file_id=AS02047.pdf Deriving the Metallicity distribution function of galactic systems ]</ref><ref name=Frenchaboy>[http://cdsweb.cern.ch/record/529715/files/0112169.pdf The Metallicity Distribution Function of ω Centauri]</ref><ref name=Halo-Beers-2005>[http://arxiv.org/abs/astro-ph/0508423 The Metallicity Distribution Function of the Halo of the Milky Way]</ref><ref name=M31-Sarajedini-2005>[http://arxiv.org/abs/astro-ph/0506653 The Metallicity Distribution Function of Field Stars in M31's Bulge]</ref><ref name=Shlesinger-2011>[http://arxiv.org/abs/1112.2214 The Metallicity Distribution Functions of SEGUE G and K dwarfs: Constraints for Disk Chemical Evolution and Formation]</ref><ref name=Yong2012>[http://arxiv.org/abs/1208.3016 The Most Metal-Poor Stars. III. The Metallicity Distribution Function and CEMP Fraction]</ref> Much of the iron in a star will have come from earlier type 1a [[supernova]]e. Other [alpha] metals will have been produced in core collapse supernovae.<ref>[http://www.astro.bas.bg/~petrov/holzman07_files/ay616/node5.html Chemical evolution models]</ref>
==References==
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