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The chemical composition of early-B type stars in Ori OB1 (Cunha & Lambert 1994) The higher values of the O abundances are found for stars in the youngest groups (Id and some Ic) O and Si abundances are correlated Coherent with a scenario of induced star formation in which the new generation of stars are formed from insterstellar material contaminated by type-II SN ejecta (O, Si, ...)
(Comparison with the O abundance content in the Orion nebula) Oxygen abundance in M42 (Esteban et al. 2004) • Preferred diagnostic lines: ORL • O depleted on to dust grains by a factor of 0.08 dex (Esteban et al. 1998) ORL + DUST
Page 2 and 3: The Orion Nebula (M42) Chemical com
Page 4 and 5: Why is interesting to investigate T
Page 6 and 7: Why is interesting to investigate T
Page 8 and 9: Chemical abundance studies of early
Page 12 and 13: The chemical composition of early-B
Page 14 and 15: How to perform a stellar abundance
Page 16 and 17: How to perform a stellar abundance
Page 18 and 19: What is new/different between CL94
Page 20 and 21: A new analysis of the B-type stars
Page 34 and 35: The chemical composition of early-B
Page 38 and 39: Conclusions - Recent accurate abund
Page 40 and 41: Orion OB1: B-type stars vs nebular

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