2002A&A...391..253F


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST22:17:16

2002A&A...391..253F - Astronomy and Astrophysics, volume 391, 253-265 (2002/8-3)

Lithium abundances from the 6104Å line in cool Pleiades stars.

FORD A., JEFFRIES R.D. and SMALLEY B.

Abstract (from CDS):

Lithium abundances determined by spectral synthesis from both the 6708Å resonance line and the 6104Å subordinate line are reported for 11 Pleiades late-G and early-K stars observed at the William Herschel Telescope. Firm detections of the weak subordinate line are found for four objects, marginal detections for four, and upper limits for the remaining three stars. Some of these spectra were previously analysed by Russell (1996ApJ...463..593R), where he reported that abundances derived from the 6104Å line were systematically higher than those obtained from the 6708Å line by 0.2-0.7dex. He also reported a reduced spread in the 6104Å line abundances compared with those determined from the 6708Å feature. Using spectral synthesis we have re-analysed Russell's data, along with our own. Our results do not entirely support Russell's conclusions. We report a ∼0.7dex scatter in the abundances from 6708Å and a scatter at least as large from the 6104Å line. We find that this is partly explained by our inclusion of a nearby FeII line and careful modelling of damping wings in the strong metal lines close to the 6104Å feature; neglect of these leads to overestimates of the Li abundance which are most severe in those objects with the weakest 6104Å lines, thus reducing the abundance scatter. We find a reasonable correlation between the 6104Å and 6708Å Li abundances, although four stars have 6104Å-determined abundances which are significantly larger than the 6708Å-determined values by up to 0.5dex, suggesting problems with the homogeneous, 1-dimensional atmospheres being used. We show that these discrepancies can be explained, although probably not uniquely, by the presence of star spots with plausible coverage fractions. The addition of spots does not significantly reduce the apparent scatter in Li abundances, leaving open the possibility that at least some of the spread is caused by real star-to-star differences in pre-main sequence Li depletion.

Abstract Copyright:

Journal keyword(s): stars: abundances - stars: late type - stars: interiors - open clusters and associations: individual: Pleiades

Simbad objects: 17

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Number of rows : 17

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 TYC 1803-616-1 PM* 03 40 30.7208255756 +24 29 14.310109841   12.592 11.716   10.753 ~ 28 0
2 TYC 1799-1268-1 PM* 03 43 34.4114059617 +23 45 42.924015073 12.914 12.35 11.47     G8V 36 0
3 HD 23195 SB* 03 43 58.8029011901 +23 52 57.828488692   10.19 9.55     ~ 67 0
4 V* V1168 Tau BY* 03 44 04.8393546146 +24 16 31.874779484   12.42 11.54     G4 56 0
5 V* V1038 Tau BY* 03 44 20.0899109759 +24 47 46.204314184   11.2 10.4 10.3   G1-2V 105 0
6 TYC 1803-1170-1 PM* 03 44 43.1747997077 +25 52 31.893226539   12.561 11.684   10.713 ~ 17 0
7 TYC 1799-272-1 SB* 03 45 03.2766667427 +23 50 21.886008398   12.87 11.93   10.97 K2V 59 0
8 BD+23 514 PM* 03 45 41.8551897178 +24 25 53.456111559   12.08 11.36 11.15 10.42 G5 48 0
9 Cl* Melotte 22 DH 462 PM* 03 46 37.7719272739 +24 44 51.680114556   12.80 11.92   10.89 K0V 44 0
10 HD 23511 PM* 03 46 39.3333752913 +24 06 11.531106899   9.75 9.28   8.75 F5V 96 0
11 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 2979 0
12 Cl* Melotte 22 PELS 143 * 03 47 57.5967610646 +26 37 45.348112355   12.528 11.655   10.728 ~ 13 0
13 Cl Melotte 22 2106 * 03 48 58.4863942051 +23 12 04.243838424   12.39 11.53   10.59 K0V 35 0
14 V* V1089 Tau BY* 03 49 24.0458986758 +23 50 21.287818903   12.13 11.35     ~ 43 0
15 Cl Melotte 22 2311 PM* 03 49 28.7424934961 +23 42 43.883161612   12.19 11.36   10.50 ~ 50 0
16 NGC 2682 OpC 08 51 18 +11 48.0           ~ 2032 0
17 BD+22 4409 BY* 21 31 01.7141405072 +23 20 07.370852589   10.28 9.253 8.6 7.965 K3Vke 152 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-22:17:16

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