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Abundance difference between components of wide binaries. II. The southern sample
Aims.We present high-precision iron abundance differences for 33 widebinaries with similar components. They were observed with the FEROSspectrograph at ESO, looking for abundance anomalies due to theingestion of metal rich material of a planetary origin. Methods:.An optimized data analysis technique and the high quality of thespectra allowed us to achieve an error of about 0.02 dex for pairs withsmall temperaure differences. Results: . We found one case (HIP64030 = HD 113984) with a large (0.27 dex) abundance difference. Theprimary of this binary appears to be a blue straggler, and the abundancedifference might be due to the peculiar evolution of the star. A fewother pairs show small abundance differences (≤0.09 dex). In a fewcases these differences suggest the ingestion of a small amount of metalrich material, but in others they are likely spurious, because of thelarge temperature difference, high level of magnetic activity, ordifferent evolutionary phases between the components. Some cases ofabundance 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 targetswould be welcome. Conclusions: . This study confirms ourpreliminary result based on analysis of 23 pairs (Desidera et al. 2004)that the occurrence of large alterations in stellar abundances caused bythe ingestion of metal rich, rocky material is not a common event. Forat least 65% of the pairs with components warmer than 5500 K, the limitson the amount of rocky material accreted by the program stars arecomparable to the estimates of rocky material accreted by the Sun duringits main-sequence lifetime.
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| Takýmyýldýz: | Kurt |
| Sað Açýklýk: | 15h12m45.37s |
| Yükselim: | -46°53'44.5" |
| Görünürdeki Parlaklýk: | 8.805 |
| Uzaklýk: | 271.003 parsek |
| özdevim Sað Açýklýk: | -6.4 |
| özdevim Yükselim: | -8.2 |
| B-T magnitude: | 9.989 |
| V-T magnitude: | 8.903 |
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