Metallicity distribution function: Difference between revisions

Revision as of 14:46, 26 January 2018

Revision as of 03:04, 16 March 2018

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</ref><ref name=M31-Sarajedini-2005>[https://arxiv.org/abs/astro-ph/0506653 The Metallicity Distribution Function of Field Stars in M31's Bulge]

</ref><ref name=Shlesinger-2011>[https://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>{{cite journal|url=https://arxiv.org/abs/1208.3016|title=The Most Metal-Poor Stars. III. The Metallicity Distribution Function and CEMP Fraction|first1=David|last1=Yong|first2=John E.|last2=Norris|first3=M. S.|last3=Bessell|first4=N.|last4=Christlieb|first5=M.|last5=Asplund|first6=Timothy C.|last6=Beers|first7=P. S.|last7=Barklem|first8=Anna|last8=Frebel|first9=S. G.|last9=Ryan|date=1 January 2013|publisher=|volume=762|issue=1|pages=27|accessdate=3 March 2017|via=arXiv.org|doi=10.1088/0004-637X/762/1/27|arxiv = 1208.3016 |bibcode = 2013ApJ...762...27Y }}</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>{{cite web|url=http://www.astro.bas.bg/~petrov/holzman07_files/ay616/node5.html|title=Chemical evolution models|work=bas.bg|accessdate=3 March 2017}}</ref><ref>{{Cite journal|arxiv=1106.2168|title=<nowiki>The [Fe/H], [C/Fe], and [alpha/Fe] distributions of the Bootes I Dwarf Spheroidal Galaxy</nowiki>|journal=The Astrophysical Journal|volume=738|pages=51|last1= Lai|first1=David K.|author2=Young Sun Lee|last3=Bolte|first3=Michael|last4=Lucatello|first4=Sara|last5= Beers|first5=Timothy C.|last6= Johnson|first6=Jennifer A.|last7=Sivarani|first7=Thirupathi|last8= Rockosi|first8=Constance M.|author-link8=Constance M. Rockosi|year=2011|doi=10.1088/0004-637X/738/1/51|bibcode = 2011ApJ...738...51L }}</ref>