Metallicity distribution function
The metallicity distribution function is an important concept in
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
- S2CID 9965955.
- S2CID 56118016.
- Bibcode:2002ASPC..265..143F.
- S2CID 18380786.
- S2CID 17051527.
- S2CID 119205318.
- S2CID 16930550.
- ^ "Chemical evolution models". bas.bg. Retrieved 3 March 2017.
- S2CID 118627008.
Further reading
- McWilliam, Andrew. (2003). Abundance ratios and galactic chemical evolution. Annual Review of Astronomy and Astrophysics. 35. 503–556. .