Investor Presentaiton

Planets vs. Metallicity In solar-type stars, more metal-rich stars are known to have more planets. In core-accretion scenario, solid cores of planets easily form in metal-rich circumstellar disks. In planet-hosting giants, however, no such metal-rich tendency has been seen so far. Efficient inward migration of planets in metal-rich disks or metallicity independent formation such as gravitational instability in disks or dilution by convective envelope? Relative Frequency Relative Frequency 0.26 Solar-type stars 0.2 .15 Ew/o planets 0.1 0.05 سیلسیلیلی w/ planets -0.5 0.5 [Fe/H Santos et al. 2004 0.4 Giant stars w/o planets] 0.3 (309) OAO Sample 0.2 w/ planets 0.1 (13) -1 -0.5 0 [Fe/H] 0.5 Takeda et al. 2008

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