2002A&A...393..617F


Query : 2002A&A...393..617F

2002A&A...393..617F - Astronomy and Astrophysics, volume 393, 617-628 (2002/10-2)

Lithium 6104 Å in Population II stars.

FORD A., JEFFRIES R.D., SMALLEY B., RYAN S.G., AOKI W., KAWANOMOTO S., JAMES D.J. and BARNES J.R.

Abstract (from CDS):

We have obtained echelle spectroscopy of 14 Population II objects selected from those previously observed by Bonifacio & Molaro (1997MNRAS.285..847B). For one object, HD 140283, we obtained exquisite data with the High Dispersion Spectrograph on the Subaru Telescope, with S/N exceeding 1000 per 0.018Å pixel. Li abundances have been determined by spectral synthesis from both the 6708Å resonance line and also from 6104Å subordinate feature. Firm detections of the weak line have been made in seven objects, and upper limits are reported for the remainder. Our 6708Å abundances agree with those reported by Bonifacio & Molaro (1997MNRAS.285..847B) with a mean difference of only 0.019±0.009dex. Abundances from the 6104Å line hint at a higher Li abundance than that determined from the resonance feature, but this evidence is mixed; the weakness of the 6104Å line and the large number of upper limits make it difficult to draw firm conclusions. NLTE-corrections increase (rather than eliminate) the size of the (potential) discrepancy, and binarity appears unlikely to affect any abundance difference. The effect of multi-dimensional atmospheres on the line abundances was also considered, although it appears that use of 3-D (LTE) models could again act to increase the discrepancy, if one is indeed present.

Abstract Copyright:

Journal keyword(s): stars: abundances - stars: Population II - stars: interiors

Simbad objects: 21

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Number of rows : 21
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 HD 24289 PM* 03 51 54.5431655808 -03 49 10.687742472   10.48 9.96     F0V 69 0
2 HD 284248 PM* 04 14 35.5161858536 +22 21 04.252516252 9.49 9.68 9.23 8.77 8.43 sdG0 177 0
3 HD 28428 * 04 27 40.6481258304 -32 24 31.124030652   7.53 7.07     F3IV 29 0
4 HD 64090 PM* 07 53 33.1208795337 +30 36 18.256204963 8.75 8.86 8.25 7.70 7.30 K0:V_Fe-3 354 0
5 HD 74000 PM* 08 40 50.8036114756 -16 20 42.516208237 9.84 10.09 9.66     F2 261 0
6 Ross 889 Pe* 09 40 43.2053340378 +01 00 29.511836741       10.39   sdA4 159 0
7 HD 83769 ** 09 40 45.78636 +01 01 29.0180   10.53 10.15 10.12   sdF5 64 0
8 HD 84937 Pe* 09 48 56.0992891997 +13 44 39.326709913 8.49 8.68 8.32 7.97 7.70 F8Vm-5 771 0
9 G 49-29 PM* 09 55 49.8273034392 +26 41 14.890852788   13.19 12.03 11.65   ~ 7 0
10 G 162-62 PM* 10 30 13.6016083230 -03 55 57.535538452   16.0       ~ 7 0
11 HD 94028 PM* 10 51 28.1256073369 +20 16 38.965439278 8.51 8.69 8.22 7.82 7.54 F8 352 0
12 HD 108177 PM* 12 25 34.9568267745 +01 17 02.259553591 9.87 10.09 9.66 9.21 8.89 F0V 246 0
13 BD-10 4091 * 15 22 54.1698175224 -10 54 47.247695892   11.002 9.81     ~ 5 0
14 HD 140283 Pe* 15 43 03.0971190219 -10 56 00.595693188 7.508 7.711 7.212 6.63 8.21 F9VkA5mA1 908 0
15 HD 230938 PM* 19 14 05.9810612376 +11 48 37.869280884       10.3   G2wl 12 0
16 HD 188510 PM* 19 55 09.6782304000 +10 44 27.398607828 9.30 9.41   8.5   G5V: 247 0
17 HD 193901 PM* 20 23 35.8471605389 -21 22 14.226959304 9.08 9.22 8.67 8.17 7.87 F7V 276 0
18 HD 194598 PM* 20 26 11.9183775668 +09 27 00.429558608 8.62 8.82 8.34 7.90 7.56 F8 297 0
19 HD 201891 Pe* 21 11 59.0321495469 +17 43 39.890919730 7.74 7.88 7.37 6.91 6.59 G5V_Fe-2.5 386 0
20 HD 219617 ** 23 17 05.04375 -13 51 03.5971 8.41 8.60 8.14 7.70 7.37 F8 307 0
21 G 273-11 PM* 23 19 02.8531634400 -17 21 19.424870352   15.995 14.486 14.334   ~ 3 0

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2023.04.01-19:41:51

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