We have modeled irradiated planets located near a dM5 and a G2 primary star .
The impinging radiation field was explicitly included in the solution of the radiative transfer equation and in the computation of the atmospheric structure .
We find that large errors in both the thermal and reflected flux will result from models which do not include the impinging radiation in a self-consistent manner .
A cool ( { T } _ { eff } = 500 K ) and a hot ( { T } _ { eff } = 1000 { K } ) planet were modeled at various orbital separations from both the dM5 and the G2 primary .
In all scenarios , we compared the effects of the irradiation in two extreme cases : one where dust clouds form and remain suspended in the atmosphere , and another where dust clouds form but completely settle out of the atmosphere .
The atmospheric structure and emergent spectrum strongly depend on the presence or absence of dust clouds .
We find that , in the absence of dust opacity , the impinging radiation significantly alters the innermost layers of an EGP atmosphere and that they are actually brighter in the optical than dusty planets .
Our models also indicate that the planet-to-star brightness ratio in the optical will be less that 1 \times 10 ^ { -5 } for objects like \tau böotis which is consistent with recently reported upper limit values .