Metallicity distribution function
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
- ^ Deriving the Metallicity distribution function of galactic systems
- ^ The Metallicity Distribution Function in the disc of the Milky Way and near the Sun
- ^ The Metallicity Distribution Function of ω Centauri
- ^ The Metallicity Distribution Function of the Halo of the Milky Way
- ^ The Metallicity Distribution Function of Field Stars in M31's Bulge
- ^ The Metallicity Distribution Functions of SEGUE G and K dwarfs: Constraints for Disk Chemical Evolution and Formation
- ^ The Most Metal-Poor Stars. III. The Metallicity Distribution Function and CEMP Fraction
- ^ Chemical evolution models
- ^ 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: 51. arXiv:1106.2168. doi:10.1088/0004-637X/738/1/51.
Further reading
 | This astronomy-related article is a stub. You can help Wikipedia by expanding it. |