The metallicity distribution function is an important concept in 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. [1][2][3][4][5][6][7]

MDFs are used to test different theories of galactic evolution. Much of the iron in a star will have come from earlier type Ia supernovae. Other [alpha] metals can be produced in core collapse supernovae.[8][9]

References

  1. ↑ Fenner, Yeshe; Gibson, Brad K. (5 March 2013). "Deriving the Metallicity Distribution Function of Galactic Systems" (PDF). Publications of the Astronomical Society of Australia. 20 (2): 189–195. arXiv:astro-ph/0304320. Bibcode:2003PASA...20..189F. doi:10.1071/AS02047. S2CID 9965955.
  2. ↑ Casagrande, L.; Schönrich, R.; Asplund, M.; Cassisi, S.; Ramírez, I.; Meléndez, J.; Bensby, T.; Feltzing, S. (26 May 2011). "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s)" (PDF). Astronomy & Astrophysics. 530: A138. arXiv:1103.4651. Bibcode:2011A&A...530A.138C. doi:10.1051/0004-6361/201016276. S2CID 56118016.
  3. ↑ Frinchaboy, P. M.; Rhee, J.; Ostheimer, J. C.; Majewski, S. R.; Patterson, R. J.; Johnson, W. Y.; Dinescu, D. I.; Palma, C.; Westfall, K. B. (2002). "The Metallicity Distribution Function of omega Centauri". Omega Centauri. 265: 143. arXiv:astro-ph/0112169. Bibcode:2002ASPC..265..143F.
  4. ↑ Beers, Timothy C; Christlieb, Norbert; Norris, John E; Bessell, Michael S; Wilhelm, Ronald; Carlos Allende Prieto; Yanny, Brian; Rockosi, Constance; Heidi Jo Newberg; Rossi, Silvia; Young Sun Lee (2005). "The Metallicity Distribution Function of the Halo of the Milky Way". Proceedings of the International Astronomical Union. 1: 175–183. arXiv:astro-ph/0508423. Bibcode:2005IAUS..228..175B. doi:10.1017/S1743921305005521. S2CID 18380786.
  5. ↑ Sarajedini, Ata; Jablonka, Pascale (2005). "The Metallicity Distribution Function of Field Stars in M31's Bulge". The Astronomical Journal. 130 (4): 1627–1634. arXiv:astro-ph/0506653. Bibcode:2005AJ....130.1627S. doi:10.1086/433171. S2CID 17051527.
  6. ↑ Schlesinger, Katharine J; Johnson, Jennifer A; Rockosi, Constance M; Young Sun Lee; Morrison, Heather L; Schoenrich, Ralph; Carlos Allende Prieto; Beers, Timothy C; Yanny, Brian; Harding, Paul; Schneider, Donald P; Chiappini, Cristina; da Costa, Luiz N; Maia, Marcio A. G; Minchev, Ivan; Rocha-Pinto, Helio; Santiago, Basilio X (2011). "The Metallicity Distribution Functions of SEGUE G and K dwarfs: Constraints for Disk Chemical Evolution and Formation". The Astrophysical Journal. 761 (2): 160. arXiv:1112.2214. Bibcode:2012ApJ...761..160S. doi:10.1088/0004-637X/761/2/160. S2CID 119205318.
  7. ↑ Yong, David; Norris, John E.; Bessell, M. S.; Christlieb, N.; Asplund, M.; Beers, Timothy C.; Barklem, P. S.; Frebel, Anna; Ryan, S. G. (1 January 2013). "The Most Metal-Poor Stars. III. The Metallicity Distribution Function and CEMP Fraction". The Astrophysical Journal. 762 (1): 27. arXiv:1208.3016. Bibcode:2013ApJ...762...27Y. doi:10.1088/0004-637X/762/1/27. S2CID 16930550.
  8. ↑ "Chemical evolution models". bas.bg. Retrieved 3 March 2017.
  9. ↑ Lai, David K.; Young Sun Lee; Bolte, Michael; Lucatello, Sara; Beers, Timothy C.; Johnson, Jennifer A.; Sivarani, Thirupathi; Rockosi, Constance M. (2011). "The [Fe/H], [C/Fe], and [alpha/Fe] distributions of the Bootes I Dwarf Spheroidal Galaxy". The Astrophysical Journal. 738 (1): 51. arXiv:1106.2168. Bibcode:2011ApJ...738...51L. doi:10.1088/0004-637X/738/1/51. S2CID 118627008.

Further reading


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