The abundance distribution of stars with planets
We present the results of a uniform, high-precision spectroscopic metallicity study of 136 G-type stars from the Anglo-Australian Planet Search, 20 of which are known to harbour extrasolar planets (as at 2005 July). Abundances in Fe, C, Na, Al, Si, Ca, Ti and Ni are presented, along with Strömgen photometric metallicities. This study is one of several recent studies examining the metallicities of a sample of planet-host and non-planet-host stars that were obtained from a single sample, and analysed in an identical manner, providing an unbiased estimate of the metallicity trends for planet-bearing stars. We find that non-parametric tests of the distribution of metallicities for planet-host and non-planet-host stars are significantly different at a level of 99.4 per cent confidence. We confirm the previously observed trend for planet-host stars to have higher mean metallicities than non-planet-host stars, with a mean metallicity for planet-host stars of [Fe/H]= 0.06 ± 0.03 dex compared with [Fe/H]=−0.09 ± 0.01 dex for non-host-stars in our sample. This enrichment is also seen in the other elements studied. Based on our findings, we suggest that this observed enhancement is more likely a relic of the original gas cloud from which the star and its planets formed, rather than being due to ‘pollution’ of the stellar photosphere.
Document Type: Research Article
Affiliations: 1: Anglo-Australian Observatory, PO Box 296, Epping, NSW 1710, Australia 2: Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road NW, Washington, DC 20015-1305, USA 3: Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB 4: Department of Astronomy, University of California, Berkeley, CA 94720, USA 5: Rutherford Appleton Laboratory, Chilton, Didcot, Oxon OX11 0QX 6: Faculty of Sciences, University of Southern Queensland, Toowoomba 4350, Australia
Publication date: July 21, 2006