The Metallicity distribution function is an important concept in stellar evolution. Often characterised as [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]
References
- ^ Deriving the Metallicity distribution function of galactic systems
- ^ 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
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