TY - GEN
T1 - Chemical homogeneity in the Orion Association
T2 - International Conference on Assembling the Puzzle of the Milky Way
AU - Cunha, K.
AU - Hubeny, Ivan -
AU - Lanz, T.
PY - 2012
Y1 - 2012
N2 - We present non-LTE oxygen abundances for a sample of B stars in the Orion association. The abundance calculations included non-LTE line formation and used fully blanketed non-LTE model atmospheres. The stellar parameters were the same as adopted in the previous study by Cunha & Lambert (1994). We find that the young Orion stars in this sample of 10 stars are described by a single oxygen abundance with an average value of A(O) = 8.78 and a small dispersion of ±0.05, dex which is of the order of the uncertainties in the analysis. This average oxygen abundance compares well with the average oxygen abundance obtained previously in Cunha & Lambert (1994): A(O) = 8.72 ± 0.13 although this earlier study, based upon non-blanketed model atmospheres in LTE, displayed larger scatter. Small scatter of chemical abundances in Orion B stars had also been found in our previous studies for neon and argon; all based on the same effective temperature scale. The derived oxygen abundance distribution for the Orion association compares well with other results for the oxygen abundance in the solar neighborhood.
AB - We present non-LTE oxygen abundances for a sample of B stars in the Orion association. The abundance calculations included non-LTE line formation and used fully blanketed non-LTE model atmospheres. The stellar parameters were the same as adopted in the previous study by Cunha & Lambert (1994). We find that the young Orion stars in this sample of 10 stars are described by a single oxygen abundance with an average value of A(O) = 8.78 and a small dispersion of ±0.05, dex which is of the order of the uncertainties in the analysis. This average oxygen abundance compares well with the average oxygen abundance obtained previously in Cunha & Lambert (1994): A(O) = 8.72 ± 0.13 although this earlier study, based upon non-blanketed model atmospheres in LTE, displayed larger scatter. Small scatter of chemical abundances in Orion B stars had also been found in our previous studies for neon and argon; all based on the same effective temperature scale. The derived oxygen abundance distribution for the Orion association compares well with other results for the oxygen abundance in the solar neighborhood.
UR - http://www.scopus.com/inward/record.url?scp=84873547206&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84873547206&partnerID=8YFLogxK
U2 - 10.1051/epjconf/20121908005
DO - 10.1051/epjconf/20121908005
M3 - Conference contribution
AN - SCOPUS:84873547206
SN - 9782759807185
T3 - EPJ Web of Conferences
BT - Assembling the Puzzle of the Milky Way
Y2 - 17 April 2011 through 22 April 2011
ER -