  Currently, there are about 3 dozen known super-Earth (M < 10 MEarth), of
which 8 are transiting planets suitable for atmospheric follow-up observations.
Some of the planets are exposed to extreme temperatures as they orbit close to
their host stars, e.g., CoRot-7b, and all of these planets have equilibrium
temperatures significantly hotter than the Earth. Such planets can develop
atmospheres through (partial) vaporization of their crustal and/or mantle
silicates. We investigated the chemical equilibrium composition of such heated
systems from 500 - 4000 K and total pressures from 10-6 to 10+2 bars. The major
gases are H2O and CO2 over broad temperature and pressure ranges, and Na, K,
O2, SiO, and O at high temperatures and low pressures. We discuss the
differences in atmospheric composition arising from vaporization of SiO2-rich
(i.e., felsic) silicates (like Earth's continental crust) and MgO-, FeO-rich
(i.e., mafic) silicates like the bulk silicate Earth. The computational results
will be useful in planning spectroscopic studies of the atmospheres of
Earth-like exoplanets.
