  We assume that the supersymmetric lightest neutralino is a good candidate for
the CDM and explore the possibility to produce diffuse radio emission from
high-energy electrons arising from the neutralino annihilation in galaxy
clusters whose intracluster medium is filled with a large-scale magnetic field.
We show that these electrons fit the population of seed relativistic electrons
postulated in many models for the origin of cluster radio halos. For magnetic
fields with central values $3 \div 30$ $\mu$G (depending on the DM profile),
the population of seed relativistic electrons from neutralino annihilation can
fit the radio halo spectra of Coma and 1E0657-56. The shape and the frequency
extension of the radio halo spectra are connected with the mass and physical
composition of the neutralino. A pure-gaugino neutralino with mass $M_{\chi}
\geq 80$ GeV can reasonably fit the spectra of both Coma and 1E0657-56. This
model provides a number of extra predictions that make it definitely testable.
On the one hand, it agrees with the observations that {\it (i)} the radio halo
is centered on the cluster dynamical center, usually coincident with the X-ray
center, {\it (ii)} the radio halo surface brightness is similar to the X-ray
one, and {\it (iii)} the monochromatic radio luminosity at 1.4 GHz correlates
strongly with the IC gas temperature. On the other hand, the model predicts
that radio halos should be present in every cluster, which is not actually
observed, although the predicted radio halo luminosities can change by a large
amount ($\sim 10^2 \div 10^6$), depending on the amplitude and the structure of
the IC magnetic field. Also, neutral pions arising from neutralino annihilation
should give rise to substantial gamma-ray emission that could be tested by the
next generation gamma-ray experiments.
