More and more observational and theoretical evidence has shown the existence of a chromospheric condensation during solar flares. Can such a chromospheric condensation play a role in the energy process of the chromospheric flare? In this paper, we have empirically studied the influence of the chromospheric condensation on the distribution of the atmospheric radiative loss. The main results are as follows: when the temperature of the condensation is lower than that below it, the radiative loss changes only slightly; but if the temperature of the condensation is higher than that below it, the radiative loss may change greatly both in the chromosphere and in the photosphere; the backwarming of the atmosphere due to the condensation may be very effective; the temperature increase in the temperature minimum region (TMR) may be as much as 500 K; and the backwarming may be effective as deep as h = 0 km, resulting in an enhancement of the continuum emission.