  In this paper we construct the interaction potential between the dense
supernova core and neutrinos due to the exchange of light radions in the
Randall-Sundrum scenario. We then show that the radion exchange potential
affects the neutrino oscillation phenomenology inside the supernova
significantly if the radion mass is less than around 1 GeV. In order that the
Bethe-Wilson mechanism for heating the envelope and r-process neucleosynthesis
be operative, the radion mass must be greater than 1 GeV. Bounds on the radion
mass of the same order of magnitude can also be derived from TASSO and CLEO
data on B decays.
