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How to perform a stellar abundance analysis: a general overview A VERY important step: stellar parameter determination Use of photometric calibrations vs. Self-consistent spectroscopic approach e.g. Lester, Gray & Kurucz (1986) [c 1 ] = c 1 – 0.20 (b-y) = f(T eff , logg) Based on Kurucz’s (1979) models T eff , logg, ... are determined by using synthetic lines resulting from the same stellar atmosphere code that will be used for the abundance analysis
How to perform a stellar abundance analysis: a general overview Abundance determination: the curve of growth method For a fixed set of stellar parameters T eff , logg, ε(He), (wind param.) i.e. a given atmosphere structure Grid of EWs of diagnostic lines (line formation code) for different [ε(X), ζ t ] – pairs
- Page 2 and 3: The Orion Nebula (M42) Chemical com
- Page 4 and 5: Why is interesting to investigate T
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- Page 8 and 9: Chemical abundance studies of early
- Page 10 and 11: The chemical composition of early-B
- Page 12 and 13: The chemical composition of early-B
- Page 14 and 15: 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 22 and 23: A new analysis of the B-type stars
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- Page 36 and 37: A new analysis of the B-type stars
- Page 38 and 39: Conclusions - Recent accurate abund
- Page 40 and 41: Orion OB1: B-type stars vs nebular
How to perform a stellar abundance analysis: a general overview<br />
Abundance determination: the curve of growth method<br />
For a fixed set of stellar parameters<br />
T eff , logg, ε(He), (wind param.)<br />
i.e. a given atmosphere structure<br />
Grid of EWs of diagnostic lines<br />
(line formation code)<br />
for different [ε(X), ζ t ] – pairs
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