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Astron. Astrophys. 322, L13-L16 (1997)

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3. Hints on LMC chemical evolution

In the LMC, spectroscopy at resolutions adequate for abundance analysis can reach only intrinsically bright objects. This severely limits our knowledge of its chemical evolution. Spectroscopic studies concern supergiant stars (Kudritzki 1988, Wolf and Reitermann 1989, Spite 1989, Russell and Bessell 1989, Spite F. et al. 1989, Spite M. et al. 1989, Richtler et al. 1989, Hill et al. 1995), B stars (Rolleston 1996), AGB stars (Frogel and Blanco 1990), planetary nebulae (Dennefeld, 1989) and HII regions (Dufour, 1984). The range in [Me/H] found is from -1.4 to -0.2, with some tendency for the youngest objects to be more metal-rich. While interesting for the objects studied, these data only shed limited light on the chemical evolution of the galaxy as a whole.

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© European Southern Observatory (ESO) 1997

Online publication: June 5, 1998

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