1997PASP..109..226C


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.06CEST01:17:21

1997PASP..109..226C - Publ. Astron. Soc. Pac., 109, 226-235 (1997/March-0)

Oxygen abundances in metal poor subgiant stars from the O I triplet.

CAVALLO R.M., PILACHOWSKI C.A. and REBOLO R.

Abstract (from CDS):

This paper examines the oxygen abundance of 24 main-sequence turn-off and subgiant stars through the permitted O I triplet near λ7774 Å. In agreement with prior investigators, we find that the O abundance from the triplet is about 0.53 dex higher than is typically found from other means such as the [O I] λ6300 Å line or the UV and IR bands from OH. Our average [O/Fe] is +0.79 ± 0.29 (1 σ), with the uncertainties in the individual methods being dominated by systematic errors in our incomplete understanding of the formation of these high excitation lines under non-LTE conditions. Several methods of resolving the on-going discrepancy are discussed in detail. We find that the problem is not fixed by simply changing the model atmosphere parameters, and that the best methods seem to require a detailed non-LTE analysis based on both the structure of the oxygen atom and the source function within and above the photosphere. The trend of increasing O with decreasing Fe is briefly explored and is found to be qualitatively consistent with other works.

Abstract Copyright:

Journal keyword(s): Stars

Simbad objects: 24

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Number of rows : 24

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 BD+37 1458 PM* 06 16 01.5222776277 +37 43 18.756795213 9.41 9.52 8.92 8.34 7.91 G0 129 0
2 HD 44007 Pe* 06 18 48.5271098810 -14 50 43.424752212   8.85 8.06 7.69   G5(IV)wF3/5 174 0
3 HD 45282 Pe* 06 26 40.7720108507 +03 25 29.794070200 8.71 8.69 8.03     Gwl 143 0
4 HD 76932 PM* 08 58 43.9328634171 -16 07 57.805389219 6.47 6.39 5.86     G2VFe-1.8CH-1 371 0
5 HD 87140 PM* 10 04 43.1807990851 +54 20 43.425447455 9.70 9.68 8.98     K0 107 0
6 HD 94028 PM* 10 51 28.1254469804 +20 16 38.965521484 8.51 8.69 8.22 7.82 7.54 F8 337 0
7 HD 97916 SB* 11 15 54.2294079228 +02 05 11.982106821 9.50 9.61   8.9   F0V 159 0
8 HD 103912 PM* 11 58 00.0820225482 +48 12 12.438186701   9.25   7.8   G5V: 66 0
9 HD 108317 Pe* 12 26 36.8316698542 +05 18 09.021203658       7.7   G2IVm-5 152 0
10 HD 111721 PM* 12 51 25.1948813622 -13 29 28.166794065   8.78 7.97     G6V 149 0
11 HD 122563 Pe* 14 02 31.8456299772 +09 41 09.942736952 7.47 7.10 6.19 5.37 4.79 G8:III:Fe-5 770 0
12 HD 128279 Pe* 14 36 48.5106582134 -29 06 46.610625293 8.64 8.63 8.00     Gw 179 0
13 BD+23 3130 Pe* 17 32 41.6248195623 +23 44 11.624030553       8.6   G0III 121 0
14 HD 163810 ** 17 58 38.4538029750 -13 05 49.654844460 10.15 10.23 9.63     G3V 139 0
15 HD 166161 PM* 18 09 40.6841408875 -08 46 45.602722086 9.53 9.13 8.16     G0wF0 133 0
16 HD 171496 * 18 36 07.4934207098 -24 26 11.312599970   9.59 8.52     G8IV 68 1
17 HD 175305 Pe* 18 47 06.4424234462 +74 43 31.448124921 8.07 7.93 7.18 6.52 6.03 G5III 200 0
18 BD+42 3187 RG* 18 54 16.9545538305 +42 59 00.382313454       9.6   G2 75 0
19 BD-18 5550 Pe* 19 58 49.7370363913 -18 12 11.142309703 10.18 10.03 9.35 9.04 8.74 CEMP-no 166 0
20 HD 189558 PM* 20 01 00.2452564415 -12 15 20.355884232   8.27 7.72     F8/G2V 175 1
21 HD 190287 PM* 20 05 38.2683033701 -34 55 11.945413960   9.23 8.54     G6Vw 58 0
22 HD 358059 Pe* 20 56 09.1348741356 -13 31 17.689533403   11.016 10.192     G0 51 0
23 HD 201889 ** 21 11 59.52350 +24 10 05.3897 8.60 8.64 8.05 7.52 7.15 G1V 151 0
24 BD+17 4708 SB* 22 11 31.3751899315 +18 05 34.158392398 9.73 9.91 9.46 9.03 8.70 sdF8 545 0

    Equat.    Gal    SGal    Ecl

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2021.05.06-01:17:21

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