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We present a detailed theoretical analysis of the local radio emission at thelower part of the solar atmosphere. To accomplish this, we have used anumerical code to simulate the emission and transport of high frequencyelectromagnetic waves from 2 GHz up to 10 THz. As initial conditions we usedthree well know chromospheric models. In this way, the generated syntheticspectra allows us to study the local emission and absorption processes withhigh resolution in both altitude and frequency. Associated with the temperatureminimum predicted by these models we found that the local optical depth atmillimeter wavelengths remains constant, producing an optically thin layerwhich is surrounded by two layers of high local emission. We call thisstructure the Chromospheric Solar Millimeter-wave Cavity (CSMC). The CSMC showsthe complexity of the relationship between the theoretical temperature profileand the observed brightness temperature and may help to understand thedispersion of the observed brightness temperature in the millimeter wavelengthrange.

The Chromospheric Solar Millimeter-wave Cavity, as a Result of the Temperature Minimum Region