2010A&A...510A..50S


Query : 2010A&A...510A..50S

2010A&A...510A..50S - Astronomy and Astrophysics, volume 510, A50-50 (2010/2-1)

Beryllium abundances along the evolutionary sequence of the open cluster IC 4651 - a new test for hydrodynamical stellar models.

SMILJANIC R., PASQUINI L., CHARBONNEL C. and LAGARDE N.

Abstract (from CDS):

Previous analyses of lithium abundances in main sequence and red giant stars have revealed the action of mixing mechanisms other than convection in stellar interiors. Beryllium abundances in stars with Li abundance determinations can offer valuable complementary information on the nature of these mechanisms. Our aim is to derive Be abundances along the whole evolutionary sequence of an open cluster. We focus on the well-studied open cluster IC 4651. These Be abundances are used with previously determined Li abundances, in the same sample stars, to investigate the mixing mechanisms in a range of stellar masses and evolutionary stages. Atmospheric parameters were adopted from a previous abundance analysis by the same authors. New Be abundances have been determined from high-resolution, high signal-to-noise UVES spectra using spectrum synthesis and model atmospheres. The careful synthetic modeling of the Be lines region is used to calculate reliable abundances in rapidly rotating stars. The observed behavior of Be and Li is compared to theoretical predictions from stellar models including rotation-induced mixing, internal gravity waves, atomic diffusion, and thermohaline mixing. Beryllium is detected in all the main sequence and turn-off sample stars, both slow- and fast-rotating stars, including the Li-dip stars, but is not detected in the red giants. Confirming previous results, we find that the Li dip is also a Be dip, although the depletion of Be is more modest than for Li in the corresponding effective temperature range. For post-main-sequence stars, the Be dilution starts earlier within the Hertzsprung gap than expected from classical predictions, as does the Li dilution. A clear dispersion in the Be abundances is also observed. Theoretical stellar models including the hydrodynamical transport processes mentioned above are able to reproduce all the observed features well. These results show a good theoretical understanding of the Li and Be behavior along the color-magnitude diagram of this intermediate-age cluster for stars more massive than 1.2M.

Abstract Copyright:

Journal keyword(s): stars: abundances - stars: evolution - rotation - open clusters and associations: individual: IC 4651

Simbad objects: 31

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Number of rows : 31
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 Cl Melotte 25 OpC 04 29 47 +16 56.9           ~ 2912 0
2 NGC 2516 OpC 07 58 06 -60 48.0           ~ 663 0
3 NGC 2632 OpC 08 40 13 +19 37.3           ~ 1434 0
4 IC 2391 OpC 08 41 10 -52 59.5           ~ 787 0
5 NGC 2682 OpC 08 51 23 +11 48.8           ~ 2220 0
6 NGC 3680 OpC 11 25 34 -43 14.4   8.40 7.6     ~ 304 0
7 NAME Coma Dwarf Galaxy G 12 26 59.0 +23 54 15     14.1     ~ 421 1
8 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4577 2
9 Cl* IC 4651 MEI 812 * 17 23 50.060 -49 53 43.23           ~ 1 0
10 IC 4651 199 * 17 24 30.8886839088 -50 00 53.694120564   12.66 12.061     ~ 18 0
11 IC 4651 200 * 17 24 31.9671961752 -49 59 43.223654976   14.12 13.55     ~ 13 0
12 IC 4651 201 * 17 24 32.4192470616 -49 59 20.678430624   13.66 13.117     ~ 13 0
13 IC 4651 95 * 17 24 36.8673528288 -49 55 54.692199984   13.473 12.937     ~ 14 0
14 IC 4651 109 * 17 24 37.5544633968 -49 57 51.528950064   14.10 13.424     ~ 10 0
15 CD-49 11401 * 17 24 41.5351328856 -49 59 06.472009932   11.401 10.363     ~ 35 0
16 IC 4651 174 * 17 24 42.0639726192 -49 53 02.418681516   12.99 12.381     ~ 14 0
17 IC 4651 208 * 17 24 45.0588170496 -50 00 52.258237020   13.45 12.832     ~ 12 0
18 IC 4651 77 * 17 24 46.0312725864 -49 54 51.049071684   14.09 13.53 13.48   ~ 14 0
19 CD-49 11402 * 17 24 46.7176119264 -49 54 06.987841164   12.027 10.894     ~ 36 0
20 IC 4651 26 * 17 24 48.2601172752 -49 56 37.112130024   14.293 13.699     ~ 12 0
21 IC 4651 29 * 17 24 49.4898016320 -49 57 26.935027812   12.03 10.90     K0III 30 0
22 IC 4651 OpC 17 24 51 -49 55.0           ~ 335 0
23 IC 4651 211 * 17 24 52.5648835272 -50 01 03.498216168   14.93 14.28     ~ 14 0
24 IC 4651 22 * 17 24 52.5930747384 -49 56 31.359913512   12.23 11.37     ~ 16 0
25 CD-49 11410 * 17 24 57.7608923184 -50 01 32.964118680   11.89 10.78     ~ 25 0
26 IC 4651 5 * 17 25 00.25 -49 56 38.1   14.653 14.022     ~ 10 0
27 IC 4651 64 * 17 25 01.2734914128 -49 53 52.900582092   12.81 11.989     ~ 19 0
28 IC 4651 131 * 17 25 06.2287424184 -49 59 49.963517628   12.97 12.256     ~ 19 0
29 IC 4651 52 * 17 25 12.7195980240 -49 54 55.745317080   14.43 13.743     ~ 12 0
30 IC 4651 43 * 17 25 14.2401503784 -49 56 43.669147992   14.89 14.193     ~ 20 0
31 IC 4651 142 * 17 25 18.3158604888 -49 58 10.240710924   13.22 12.685     ~ 16 0

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2022.12.09-20:38:48

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