  Active galactic nuclei (AGN) powered by the central Super-Massive Black Holes
(SMBHs) play a major role in modifying the thermal properties of the
intracluster medium (ICM). In this work, we implement two AGN heating models:
(i) by buoyant cavities rising through stratified ICM (effervescent model) and,
(ii) by viscous and conductive dissipation of sound waves (acoustic model). Our
aim is to determine whether these heating models are consistent with ICM
observables and if one is preferred over the other. We assume an initial
entropy profile of ICM that is expected from the purely gravitational infall of
the gas in the potential of the dark matter halo. We then incorporate heating,
radiative cooling, and thermal conduction to study the evolution of ICM over
the age of the clusters. Our results are: (i) Both the heating processes can
produce comparable thermal profiles of the ICM with some tuning of relevant
parameters. (ii) Thermal conduction is crucially important, even at the level
of 10\% of the Spitzer values, in transferring the injected energy beyond the
central regions, and without which the temperature/entropy profiles are
unrealistically high. (iii) The required injected AGN power scales with cluster
mass as $M_{\rm vir}^{1.5}$ for both models. (iv) The required AGN luminosity
is comparable with the observed radio jet power, reinforcing the idea that AGNs
are the dominant heating source in clusters. (v) Finally, we estimate that the
fraction of the total AGN luminosity available as the AGN mechanical luminosity
at $0.02r_{500}$ is less than 0.05\%.
