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Line 9: </ref><ref name=Yong2012>[http://arxiv.org/abs/1208.3016 The Most Metal-Poor Stars. III. The Metallicity Distribution Function and CEMP Fraction]</ref> MDFs are used to test different theories of galactic evolution. Much of the iron in a star will have come from earlier type Ia [[supernova]]e. Other [alpha] metals can be produced in core collapse supernovae.<ref>[http://www.astro.bas.bg/~petrov/holzman07_files/ay616/node5.html Chemical evolution models]</ref><ref>{{cite ~~web~~arXiv \|~~url~~arxiv=~~http://arxiv.org/abs/~~1106.2168 \|title=<nowiki>The [Fe/H], [C/Fe], and [alpha/Fe] distributions of the Bootes I Dwarf Spheroidal Galaxy</nowiki>}}</ref> ==References== Line 16: ==Further reading== * [http://ned.ipac.caltech.edu/level5/March03/McWilliam/McWilliam_contents.html ABUNDANCE RATIOS AND GALACTIC CHEMICAL EVOLUTION. Andrew McWilliam. Annu. Rev. Astron. Astrophys. 1997. 35: 503-556 ] [[Category:Stellar evolution]]

Metallicity distribution function: Difference between revisions