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]
MDFs are used to test different theories of galactic evolution. Much of the iron in a star will have come from earlier type 1a supernovae. Other [alpha] metals can be produced in core collapse supernovae.[7][8]
References
- ^ Deriving the Metallicity distribution function of galactic systems
- ^ 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
- ^ "The [Fe/H], [C/Fe], and [alpha/Fe] distributions of the Bootes I Dwarf Spheroidal Galaxy".
This article has not been added to any content categories. Please help out by adding categories to it so that it can be listed with similar articles, in addition to a stub category. (November 2012) |
 | This astronomy-related article is a stub. You can help Wikipedia by expanding it. |