Hostname: page-component-5cf477f64f-54txb Total loading time: 0 Render date: 2025-04-05T22:53:29.951Z Has data issue: false hasContentIssue false
  • English
  • Français

The Chemical Evolution of the Galactic Halo and Disk

Published online by Cambridge University Press:  04 August 2017

Federico Ferrini ,
Francesco Palla  and
Steven N. Shore
Federico Ferrini
Affiliation:
Instituto di Astronomía, Universitá di Pisa, Italy
Francesco Palla
Affiliation:
Osservatorio Astrofisico, Arcetri, Firenze, Italy
Steven N. Shore
Affiliation:
Department of Physics, New Mexico Institute of Mining and Technology, Socorro, USA

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The history of star formation in our galaxy is written in the metal abundance distributions of the stellar populations. Any star formation model is constrained by two facts. First, there was a period in the early stages of galactic evolution during which the metallicity of the gas out of which stars were being formed was significantly lower than the present epoch. Second, there is a paucity of extremely metal deficient stars in the disk of the galaxy.

Type
II. Large Scale Processes of Star Formation
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 701 - 703
Copyright
Copyright © Reidel 1987 

References

Larson, R.B.: 1985, Monthly Notices Roy. Astron. Soc., in press.Google Scholar
Pagel, B.E.J., and Edmunds, M.G.: 1981, Ann. Rev. Astr. Ap. 19, 77.Google Scholar
Tinsley, B.M.: 1980, Fund. Cosm. Phys. 5, 287.Google Scholar
Twarog, B.A.: 1985, in The Milky Way, IAU Symposium No. 106, eds. van Woerden, H., Allen, R.J., and Burton, W.B., Dordrecht: D. Reidel, p. 587.Google Scholar