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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 ((), the relative abundance of iron and hydrogen) of a population of stars such as in a cluster or galaxy.
〔(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 )〕
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 () metals can be produced in core collapse supernovae.〔(Chemical evolution models )〕
==References==
抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』
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