Metallicity distribution function
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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
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Further reading
[edit | edit source]- McWilliam, Andrew. (2003). Abundance ratios and galactic chemical evolution. Annual Review of Astronomy and Astrophysics. 35. 503–556. Lua error in Module:Citation/CS1/Configuration at line 2172: attempt to index field '?' (a nil value)..
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