2002A&A...390..235N


C.D.S. - SIMBAD4 rel 1.7 - 2021.02.26CET05:51:33

2002A&A...390..235N - Astronomy and Astrophysics, volume 390, 235-251 (2002/7-4)

O/Fe in metal-poor main sequence and subgiant stars.

NISSEN P.E., PRIMAS F., ASPLUND M. and LAMBERT D.L.

Abstract (from CDS):

A study of the O/Fe ratio in metal-poor main sequence and subgiant stars is presented using the [OI]6300 Å line, the OI 7774Å triplet, and a selection of weak FeII lines observed on high-resolution spectra acquired with the VLT UVES spectrograph. The [OI] line is detected in the spectra of 18 stars with -2.4<[Fe/H]←0.5, and the triplet is observed for 15 stars with [Fe/H] ranging from -1.0 to -2.7. The abundance analysis was made first using standard model atmospheres taking into account non-LTE effects on the triplet: the [OI] line and the triplet give consistent results with [O/Fe] increasing quasi-linearly with decreasing [Fe/H] reaching [O/Fe]≃+0.7 at [Fe/H]=-2.5. This trend is in reasonable agreement with other results for [O/Fe] in metal-poor dwarfs obtained using standard atmospheres and both ultraviolet and infrared OH lines. There is also broad agreement with published results for [O/Fe] for giants obtained using standard model atmospheres and the [OI] line, and the OH infrared lines, but the OI lines give higher [O/Fe] values which may, however, fall into place when non-LTE effects are considered. When hydrodynamical model atmospheres representing stellar granulation in dwarf and subgiant stars replace standard models, the [O/Fe] from the [OI] and FeII lines is decreased by an amount which increases with decreasing [Fe/H]. These 3D effects on [O/Fe] is compounded by the opposite behaviour of the [OI] (continuous opacity effect) and FeII lines (excitation effect). The [O/Fe] vs. [Fe/H] relation remains quasi-linear extending to [O/Fe]≃+0.5 at [Fe/H]=-2.5, but with a tendency of a plateau with [O/Fe]≃+0.3 for -2.0<[Fe/H]←1.0, and a hint of cosmic scatter in [O/Fe] at [Fe/H]≃-1.0. Use of the hydrodynamical models disturbs the broad agreement between the oxygen abundances from the [OI], OI and OH lines, but 3D non-LTE effects may serve to erase these differences. The [O/Fe] values from the [OI] line and the hydrodynamical model atmospheres for dwarfs and subgiant stars are lower than the values for giants using standard model atmospheres and the [OI] and OI lines.

Abstract Copyright:

Journal keyword(s): stars: abundances - stars: atmospheres - stars: fundamental parameters - Galaxy: evolution

VizieR on-line data: <Available at CDS (J/A+A/390/235): stars.dat tablea1.dat>

Simbad objects: 41

goto Full paper

goto View the reference in ADS

Number of rows : 41

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 HD 3567 PM* 00 38 31.9476246205 -08 18 33.395481958 9.54 9.70 9.23     F7/8wF3 196 0
2 BD-10 388 PM* 01 50 32.6463515122 -09 21 02.838270707   10.78 10.37     F3 87 0
3 G 75-31 PM* 02 38 21.5034600130 +02 26 44.370026467   10.99   10.2   sd?F8 59 0
4 HD 19445 PM* 03 08 25.5884 +26 19 51.400 8.29 8.52 8.06 7.60 7.27 G2VFe-3 745 0
5 CD-57 1633 HV* 07 06 28.9517777029 -57 27 29.118056344   10.04 9.54     F7V 92 0
6 BD+24 1676 PM* 07 30 41.2663867705 +24 05 10.250742299   11.15   10.4   F 113 0
7 HD 76932 PM* 08 58 43.9328634171 -16 07 57.805389219 6.47 6.39 5.86     G2VFe-1.8CH-1 370 0
8 HD 78558 PM* 09 08 25.2378567417 -15 08 41.237446346   7.91 7.34     G0.5V 133 0
9 HD 298986 PM* 10 17 14.8775103392 -52 29 18.691601582   10.46 10.03   9.48 F5 76 0
10 HD 97320 Pe* 11 11 00.7344947834 -65 25 37.746274848   9.769 9.269     F3V 127 0
11 HD 97916 SB* 11 15 54.2294079228 +02 05 11.982106821 9.50 9.61   8.9   F0V 157 0
12 HD 99383 Pe* 11 25 49.8354897547 -38 52 16.937834236   9.56 9.08     F2V 77 0
13 HD 103095 PM* 11 52 58.7683801554 +37 43 07.240082865 7.38 7.20 6.45 5.80 5.35 K1V_Fe-1.5 754 1
14 HD 103273 * 11 53 40.7539014989 +08 34 19.904061576   8.93 7.91     G5 10 0
15 HD 103723 PM* 11 56 36.0250188318 -21 25 09.826660968   10.554 10.091     F5/6V 71 0
16 BD-04 3208 PM* 12 07 15.0719832426 -05 44 01.609304815   10.40 9.99     A7 139 0
17 HD 106038 PM* 12 12 01.3690548563 +13 15 40.620671155 10.45 10.630 10.162 9.851 9.539 F6wl 175 0
18 HD 111980 SB* 12 53 15.0528185218 -18 31 20.009066873 8.80 8.91 8.38     F7V 158 0
19 HD 113679 PM* 13 05 52.8243888123 -38 30 59.990798799   10.342 9.797     G2/3V 86 0
20 HD 116064 Pe* 13 21 43.7823913103 -39 18 39.998476883   9.26 8.81     F9IV-Vm-5 125 0
21 HD 121004 PM* 13 53 58.1163515488 -46 32 19.526169178   10.112 9.522     G2V 132 0
22 HD 122196 PM* 14 01 02.1244272306 -38 03 03.297565043   9.19 8.75     F0(V)w 110 0
23 HD 126681 PM* 14 27 24.9096361739 -18 24 40.457119166   9.939 9.535     G3V 170 0
24 HD 132475 PM* 14 59 49.7649807130 -22 00 45.814964574 8.98 9.11 8.55     F5/6V 229 1
25 HD 140283 Pe* 15 43 03.0967798658 -10 56 00.595803430 7.508 7.711 7.212 6.63 8.21 F9VkA5mA1 870 0
26 BD+23 3130 Pe* 17 32 41.6248195623 +23 44 11.624030553       8.6   G0III 120 0
27 HD 160617 PM* 17 42 49.3235999900 -40 19 15.505712142   9.18 8.73 8.394 8.065 G0 187 0
28 BD+20 3603 PM* 17 54 43.2306261669 +20 16 16.443521966   10.13   9.6   F0 151 0
29 BD+01 3597 PM* 18 07 56.5964043215 +01 52 32.700438137   11.53   10.8   sdF5 61 0
30 HD 166913 PM* 18 16 25.6833261555 -59 24 11.241154880   8.66 8.23     F5/7Vw 124 0
31 HD 175179 PM* 18 54 23.2030233107 -04 36 18.624524830 9.56 9.61 9.03     G5V 109 0
32 HD 338529 PM* 19 32 31.9104538188 +26 23 26.116678290   9.72   9.2   B5 202 0
33 HD 188510 PM* 19 55 09.6783577203 +10 44 27.395091177 9.30 9.41   8.5   G5V: 238 0
34 HD 189558 PM* 20 01 00.2452564415 -12 15 20.355884232   8.27 7.72     F8/G2V 174 1
35 HD 195633 PM* 20 32 23.9917031781 +06 31 03.251333868 9.05 9.03 8.52     G0Vw 130 0
36 LP 815-43 PM* 20 38 13.2997980664 -20 26 10.852305467   11.31 10.72     ~ 68 0
37 CD-30 18140 PM* 20 44 06.2871219229 -30 00 07.598765502   10.326 9.932     F8 79 0
38 CD-35 14849 PM* 21 33 49.75243 -35 26 14.2322   10.95 10.56 10.59   B8 65 0
39 HD 205650 PM* 21 37 26.0309417494 -27 38 06.697112156   9.59 9.00     F6V 98 0
40 BD+17 4708 SB* 22 11 31.3751899315 +18 05 34.158392398 9.73 9.91 9.46 9.03 8.70 sdF8 544 0
41 HD 213657 PM* 22 33 47.0565944504 -42 03 13.792590617   10.08 9.66     (G0)w(A) 86 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2002A&A...390..235N and select 'bookmark this link' or equivalent in the popup menu


2021.02.26-05:51:33

© Université de Strasbourg/CNRS

    • Contact