Abundance difference between components of wide binaries. II. The southern sample

Details Abundance difference between components of wide binaries. II. The southern sample Abundance difference between components of wide binaries. II. The southern sample

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006a%26a...454..581d&link_type=abstract

Astronomy and Astrophysics, Volume 454, Issue 2, August I 2006, pp.581-593

Astronomy and Astrophysics

Astrophysics

10

Stars: Abundances, Stars: Planetary Systems, Stars: Binaries: Visual, Techniques: Spectroscopic

Scientific paper

Aims.We present high-precision iron abundance differences for 33 wide binaries with similar components. They were observed with the FEROS spectrograph at ESO, looking for abundance anomalies due to the ingestion of metal rich material of a planetary origin. Methods: .An optimized data analysis technique and the high quality of the spectra allowed us to achieve an error of about 0.02 dex for pairs with small temperaure differences. Results: . We found one case (HIP 64030 = HD 113984) with a large (0.27 dex) abundance difference. The primary of this binary appears to be a blue straggler, and the abundance difference might be due to the peculiar evolution of the star. A few other pairs show small abundance differences (≤0.09 dex). In a few cases these differences suggest the ingestion of a small amount of metal rich material, but in others they are likely spurious, because of the large temperature difference, high level of magnetic activity, or different evolutionary phases between the components. Some cases of abundance differences involving pairs with warm (Teff ≥ 6000 K) primaries might be due to the diffusion of heavy elements; dedicated theoretical models for the stellar parameters of the targets would be welcome. Conclusions: . This study confirms our preliminary result based on analysis of 23 pairs (Desidera et al. 2004) that the occurrence of large alterations in stellar abundances caused by the ingestion of metal rich, rocky material is not a common event. For at least 65% of the pairs with components warmer than 5500 K, the limits on the amount of rocky material accreted by the program stars are comparable to the estimates of rocky material accreted by the Sun during its main-sequence lifetime.

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