2014A&A...562A.102O


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.02CEST13:27:32

2014A&A...562A.102O - Astronomy and Astrophysics, volume 562A, 102-102 (2014/2-1)

Abundances and possible diffusion of elements in M 67 stars.

OENEHAG A., GUSTAFSSON B. and KORN A.

Abstract (from CDS):

The rich open cluster M 67 is known to have a chemical composition close to solar and an age of about 3.5-4.8Gyr. It offers an important opportunity to check and develop our understanding of the physics and the evolution of solar-type stars. We present a spectroscopic study at high resolution, R≃50000, of 14 stars located on the main sequence, at the turn-off point, and on the early subgiant branch in the cluster in order to investigate its detailed chemical composition, for comparison with the Sun and solar twins in the solar neighbourhood, and to explore selective atomic diffusion of chemical elements as predicted by stellar-structure theory. We have obtained VLT/FLAMES-UVES spectra and analysed these strictly differentially in order to explore chemical-abundance similarities and differences between the M 67 stars and the Sun and among the M 67 stars themselves. Individual abundances of 19 different chemical elements are obtained for the stars. They are found to agree very well with solar abundances, with abundance ratios closer to solar than those of most solar twins in the solar neighbourhood. An exception is Li, which shows considerable scatter among the cluster stars. There is a tendency for the cluster-star abundances to be more depleted than the abundances in the field stars in correlation with the condensation temperature of the elements, a tendency also found earlier for the Sun. Moreover, the heavy-element abundances are found to be reduced in the hotter stars and dwarfs by typically ≤0.05dex, as compared to the abundances of the subgiants. The results support the hypothesis that the gas of the proto-cluster was depleted by formation and cleansing of dust before the stars formed. They also add support to the proposal that the Sun was formed in a dense stellar environment. Moreover, the observed minor reductions of heavy elements, relative to our standard star M 67-1194 and the subgiants, in the atmospheres of dwarfs and turn-off point stars seem to suggest that diffusion processes are at work in these stars, although the evidence is not compelling. Based on theoretical models, the diffusion-corrected initial metallicity of M 67 is estimated to be [Fe/H]=+0.06.

Abstract Copyright:

Journal keyword(s): stars: atmospheres - stars: fundamental parameters - stars: abundances - techniques: spectroscopic - open clusters and associations: individual: M 67 - methods: observational

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 - 2020
#notes
1 NGC 2682 22 SB* 08 50 51.8289082313 +11 56 55.908491167 13.367 13.271 12.743   12.143 ~ 27 0
2 NGC 2682 31 * 08 50 56.0069423705 +11 53 51.983270222 14.289 14.205 13.634 13.586 12.986 F8V 16 0
3 NGC 2682 40 * 08 50 58.9127595806 +11 48 19.303662822 14.460 14.34 13.793   13.101 G0V 14 0
4 Cl* NGC 2682 YBP 1194 * 08 51 00.8053336097 +11 48 52.796026050 15.546 15.28 14.676   13.876 G5V 49 1
5 NGC 2682 54 V* 08 51 03.2565721431 +11 45 47.410549265 13.451 13.268 12.628   11.955 G0IV 33 0
6 Cl* NGC 2682 ES IV-37 * 08 51 05.2418231816 +11 49 34.127517590 14.444 14.314 13.739   13.093 F9V 16 0
7 NGC 2682 85 * 08 51 12.6776909559 +11 50 34.626551844 14.316 14.23 13.639   12.990 G0V 15 0
8 NGC 2682 OpC 08 51 18 +11 48.0           ~ 2032 0
9 NGC 2682 115 V* 08 51 18.5413357444 +11 49 21.514285478 13.309 13.26 12.645 12.274 11.924 F9IV 64 0
10 NGC 2682 127 V* 08 51 20.1237965086 +11 46 41.753630000 13.336 13.32 12.776   12.08 ~ 71 0
11 Cl* NGC 2682 ES III-3 V* 08 51 33.2260796838 +11 48 51.341624868 13.358 13.35 12.773   12.023 F8V 19 0
12 NGC 2682 202 V* 08 51 37.4062316298 +11 50 05.309567072 13.268 13.15 12.608   11.874 F9IV 26 0
13 NGC 2682 214 * 08 51 40.8169744404 +11 49 05.601351224 14.407 14.35 13.885   13.137 G0V 19 0
14 NGC 2682 215 V* 08 51 41.2291248775 +11 54 29.073545099 13.350 13.34 12.836   12.143 F8IV 28 0
15 NGC 2682 243 Ro* 08 51 49.9490256108 +11 49 31.201271609 13.331 13.23 12.675   11.913 F8 37 0
16 HD 101364 PM* 11 40 28.4842891594 +69 00 30.600485781   9.32 8.67     G5 64 0
17 M 4 GlC 16 23 35.22 -26 31 32.7           ~ 1676 0
18 NGC 6397 GlC 17 40 42.09 -53 40 27.6   7.39 5.17     ~ 1798 1
19 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11532 0
20 NGC 6752 GlC 19 10 52.11 -59 59 04.4   6.96 6.28     ~ 1806 0
21 * 16 Cyg A ** 19 41 48.9539315338 +50 31 30.218780803 6.79 6.59 5.95 5.50 5.17 G1.5Vb 675 1

    Equat.    Gal    SGal    Ecl

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2020.07.02-13:27:32

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