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A new analysis of the B-type stars in Ori OB1 (Simón-Díaz 2010) Stellar parameter determination: spectroscopic approach For the hotter objects: Si IV /Si III ionization balance ... and the H Balmer lines log g = 4.2 log g = 4.3 log g = 4.4 T eff =26000 ± 400 K T eff =26200 ± 400 K T eff =26500 ± 400 K
A new analysis of the B-type stars in Ori OB1 (Simón-Díaz 2010) Stellar parameter determination: spectroscopic approach ... also the He I-II ionization equilibrium (if Teff > 29000 K) HD 36512 (B0 V) H-Si analysis logg = 4.2 T eff = 33700 K H-He analysis logg = 4.2 T eff = 34000 K
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 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 22 and 23: 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

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