  Diffuse, extended radio emission in galaxy clusters, commonly referred to as
radio halos, indicate the presence of high energy cosmic ray (CR) electrons and
cluster-wide magnetic fields. We can predict from theory the expected surface
brightness of a radio halo, given magnetic field and CR density profiles.
Previous studies have shown that the nature of CR transport can radically
effect the expected radio halo emission from clusters (Wiener et al. 2013).
Reasonable levels of magnetohydrodynamic (MHD) wave damping can lead to
significant CR streaming speeds. But a careful treatment of MHD waves in a high
$\beta$ plasma, as expected in cluster environments, reveals damping rates may
be enhanced by a factor of $\beta^{1/2}$. This leads to faster CR streaming and
lower surface brightnesses than without this effect. In this work we re-examine
the simplified, 1D Coma cluster simulations (with radial magnetic fields) of
Wiener et al. (2013) and discuss observable consequences of this high $\beta$
damping. Future work is required to study this effect in more realistic
simulations.
