Metallicity distribution function: Difference between revisions

Revision as of 03:06, 16 March 2018

Revision as of 03:06, 16 March 2018

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</ref><ref name=Casagrande>[http://www.aanda.org/articles/aa/pdf/2011/06/aa16276-10.pdf The Metallicity Distribution Function in the disc of the Milky Way and near the Sun]

</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>{{Cite journal|arxiv=astro-ph/0508423|last1=Beers|first1=Timothy C|title=The Metallicity Distribution Function of the Halo of the Milky Way|journal=Proceedings of the International Astronomical Union|volume=1|pages=175|last2=Christlieb|first2=Norbert|last3=Norris|first3=John E|last4=Bessell|first4=Michael S|last5=Wilhelm|first5=Ronald|author6=Carlos Allende Prieto|last7=Yanny|first7=Brian|last8=Rockosi|first8=Constance|author9=Heidi Jo Newberg|last10=Rossi|first10=Silvia|author11=Young Sun Lee|year=2005|doi=10.1017/S1743921305005521}}</ref><ref name=M31-Sarajedini-2005>{{Cite journal|arxiv=astro-ph/0506653|last1=Sarajedini|first1=Ata|title=The Metallicity Distribution Function of Field Stars in M31's Bulge|journal=The Astronomical Journal|volume=130|issue=4|pages=1627–1634|last2=Jablonka|first2=Pascale|year=2005|doi=10.1086/433171}}</ref><ref name=Shlesinger-2011>{{Cite journal|arxiv=1112.2214|last1=Schlesinger|first1=Katharine J|title=The Metallicity Distribution Functions of SEGUE G and K dwarfs:

</ref><ref name Constraints for Disk Chemical Evolution and Formation|journal=The Astrophysical Journal|volume=761|issue=2|pages=160|last2=Johnson|first2=Jennifer A|last3=Rockosi|first3=Constance M|author4=Young Sun Lee|last5=Morrison|first5=Heather L|last6=Schoenrich|first6=Ralph|author7=Carlos Allende Prieto|last8=Halo-Beers-2005>{{cite|first8=Timothy arxivC|eprintlast9=astro-ph/0508423}}</ref><refYanny|first9=Brian|last10=Harding|first10=Paul|last11=Schneider|first11=Donald nameP|last12=M31-Sarajedini-2005>{{citeChiappini|first12=Cristina|last13=da arxivCosta|eprintfirst13=astro-ph/0506653}}</ref><refLuiz nameN|last14=Maia|first14=Marcio A. G|last15=Minchev|first15=Ivan|last16=ShlesingerRocha-2011>{{citePinto|first16=Helio|last17=Santiago|first17=Basilio arxivX|eprintyear=11122011|doi=10.22141088/0004-637X/761/2/160}}</ref><ref name=Yong2012>{{cite journal|title=The Most Metal-Poor Stars. III. The Metallicity Distribution Function and CEMP Fraction|journal=The Astrophysical Journal|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|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>