  A possibility of generating a population of cosmic-ray particles accelerated
in supernovae typeIa (SNIa) remnants in the intracluster medium (ICM) is
discussed. The presently constrained host-less SNIa rates in the clusters are
found to be sufficient to fill a few hundred kpc region with cosmic-ray
electrons within their typical synchrotron life-time of 100 Myr. The SNIa have
already been considered potential sources of excess Fe abundance in cool-core
clusters, distributed heating and turbulence in ICM. A good fraction of total
radio power from mini-halos can be sourced from the SNIa energy deposited in
the ICM with required energy conversion efficiency <1 per cent. The radio power
estimated from low Mach number shock acceleration in SNIa remnants is
consistent with the observations within the uncertainties in the estimates.
Some observational properties of the radio mini-halos are broadly consistent
with the SNIa scenario. It is also speculated that radio powers and possibly
detections of mini-halos are linked to star formation and merger histories of
the clusters.
