Taking secondary particles produced from dark matter annihilation process to thernorigin of the extended diffuse radio emissions observed in galaxy clusters, we studiedrnboth their morphology and radio spectral profile using simulated Coma like galaxyrnclusters. We have considered a neutralino annihilation channel dominated by bbrnspecies with a branching ratio of 1 and neutralino mass of 35 GeV with annihilationrncross-section times velocity value of 1_10ï¿½ï¿½26 cm3 sï¿½ï¿½1. The radio emission mapsrnproduced for the two simulated galaxy clusters which are based on the MUsicrnSImulation of galaxy Clusters (MUSIC)-dataset reveal the observed radio halornmorphology showing radio emissions both from the central regions of the clusterrnand substructures lying off-center. The flux density curve is in a good agreementrnfor _ _ 2 GHz with the obsevational values of (Thierbach et al., 2003) for the Comarncluster of galaxies showing a small deviation at higher frequencies. The smallrnspectral index fluctuations observed in the wide cluster regions corresponds to thernDM substructures scattered with in the clusters. The spectral index values _ (-0.8,rn-1.0) and _ (-1.6, -2.2) obtained in the very center and dark matter substructurern(cluster periphery) are in a good agreement with the work of (Giovannini et al.,rn1993). The central spectral flattening and the peripheral steepening explain therndense central and underdense peripheral DM regions, respectively.