  AGN feedback is now widely believed to play a crucial role in the
co-evolution between the central black hole and its host galaxy. Two feedback
modes have been identified, namely the radiative and kinetic modes, which
correspond to the luminous AGNs and low-luminosity AGNs (LLAGNs), respectively.
In this paper, we investigate the radiative heating in the kinetic mode. This
process is potentially important because: 1) the radiation power of LLAGNs is
higher than the jet power over a wide parameter range, 2) the spectral energy
distribution of LLAGNs is such that the radiative heating is more effective
compared to that of luminous AGNs with the same luminosity, and 3) most of the
time in the lifecycle of an AGN is spent in the LLAGNs phase. In this paper,
adopting the characteristic broad-band spectral energy distributions of LLAGNs,
we calculate the value of "Compton temperature" ($T_{\rm c}$), which determines
the radiative heating by Compton scattering. We find that $T_{\rm c}\sim
(5-15)\times 10^7$ K, depending on the spectrum of individual LLAGN and at
which distance from the black hole we evaluate the heating. We also compare
this heating process with other radiative heating and cooling processes such as
photoionization/recombination. Our result can be used for an accurate
calculation of the radiative heating in the study of AGN feedback.
