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We used a sample of super-Earth-like planets detected by the Dopplerspectroscopy and transit techniques to explore the dependence of orbitalparameters of the planets on the metallicity of their host stars. We confirmthe previous results (although still based on small samples of planets) thatsuper-Earths orbiting around metal-rich stars are not observed to be as distantfrom their host stars as we observe their metal-poor counterparts to be. Theorbits of these super-Earths with metal-rich hosts usually do not reach intothe Habitable Zone (HZ), keeping them very hot and inhabitable. We found thatmost of the known planets in the HZ are orbiting their GK-type hosts which aremetal-poor. The metal-poor nature of planets in the HZ suggests a high Mgabundance relative to Si and high Si abundance relative to Fe. These resultslead us to speculate that HZ planets might be more frequent in the ancientGalaxy and had compositions different from that of our Earth.

Which type of planets do we expect to observe in the Habitable Zone?