Statistics
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.0405c&link_type=abstract
American Astronomical Society, DPS meeting #40, #4.05; Bulletin of the American Astronomical Society, Vol. 40, p.392
Statistics
Scientific paper
The tendency of planets to be found preferentially around metal-rich stars is now well established. This correlation gives strong support for most planets being formed by a core accretion scenario. The situation for planets around stars with sub-solar metallicity is, however, much less clear. In the metallicity range -0.8<[Fe/H]<-0.2, the overwhelming majority of stars belong to the thin-disk, but most of the planet-hosting stars are members of the thick-disk population. One possible explanation for this is that thick-disk stars have [α-elements/Fe] significantly enhanced over thin-disk stars of the same [Fe/H]. Even among metal-rich thin-disk stars, Robinson et al. (2006) found that planet-hosting stars have show enrichment of Si and Ni over the general population. Thus, we suggest that the real key to planet formation is not the Fe abundance, but rather the total abundance of heavy elements available to form planets. We define a new total metallicity parameter ζ= log10(Z*/ZSun) (where Z is total stellar heavy element abundance), and reexamine the trends of planet discoveries as a function of ζ rather than of [Fe/H]. We also describe a new observing program to survey stars in the metallicity region which samples both thick- and thin-disk stars, in order to improve the statistics of this relationship.
Barnes Stuart
Cochran William D.
Endl Michael
MacQueen Phillip J.
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