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
- ^ "The [Fe/H], [C/Fe], and [alpha/Fe] distributions of the Bootes I Dwarf Spheroidal Galaxy".
Further reading
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