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A new analysis of the B-type stars in Ori OB1 (Simón-Díaz 2010) Oxygen abundance analysis: method and uncertainties Method: similar to Si, but only with O II lines 1) Uncertainty due to EW measurement 2) Uncertainty due to microturbulence determination 3) Uncertainty due to line dispersion 4) Uncertainty due to stellar parameter determination HD36512 logg = 4.2 T eff = 33, 34, 35 kK HD35299 logg = 4.2 T eff = 23, 24, 25 kK
A new analysis of the B-type stars in Ori OB1 (Simón-Díaz 2010) Results from the analysis: (II) O abundances Total uncertainty ∼ ± 0.08 – 0.12 dex
- 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 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 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 22 and 23: A new analysis of the B-type stars
- Page 24 and 25: A new analysis of the B-type stars
- Page 26 and 27: A new analysis of the B-type stars
- Page 30 and 31: A new analysis of the B-type stars
- Page 32 and 33: A new analysis of the B-type stars
- Page 34 and 35: The chemical composition of early-B
- 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
A new analysis of the B-type stars in Ori OB1 (Simón-Díaz 2010)<br />
Oxygen abundance analysis: method and uncertainties<br />
Method: similar to Si, but only with O II lines<br />
1) Uncertainty due to EW measurement<br />
2) Uncertainty due to microturbulence determination<br />
3) Uncertainty due to line dispersion<br />
4) Uncertainty due to stellar parameter determination<br />
HD36512 logg = 4.2 T eff = 33, 34, 35 kK HD35299 logg = 4.2 T eff = 23, 24, 25 kK
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