is generally in carbon monoxide. This is the dominant molecule of carbon for M dwarfs with of 2200-3500 K. At the highest , clouds of iron particulates can form and persist in the upper atmosphere, as may be the case in HD209458b. There are, however, significant day/night differences and unique reflective properties that distinguish a roaster from a lone and isolated edge star. Exotic general circulation models (GCMs)[@menou; @Cho03; @burk04] may soon be necessary to understand the equatorial currents, jet streams, day/night differences, terminator chemistry, and global wind dynamics of severely irradiated roasters, in particular, and of orbiting, rotating EGPs, in general.

It is useful to note that a young EGP in a wide orbit with a mass of 1.0 to 5.0 has an atmosphere and spectrum that are similar to those of an old brown dwarf with a mass of 30-60 . As it evolves, the spectroscopic class of a giant planet can transition from that of a hot M dwarf, into an L dwarf (where the silicate clouds are [*in*]{} the atmosphere), then into a T dwarf, ending up in the territory, as yet unexplored, between the Jovian planets and the “stars." If its mass is low enough, 