Thermal Instability of Halo Gas Heated by Streaming Cosmic Rays
  Heating of virialized gas by streaming cosmic rays (CRs) may be energetically
important in galaxy halos, groups and clusters. We present a linear thermal
stability analysis of plasmas heated by streaming CRs. We separately treat
equilibria with and without background gradients, and with and without gravity.
We include both CR streaming and diffusion along the magnetic-field direction.
Thermal stability depends strongly on the ratio of CR pressure to gas pressure,
which determines whether modes are isobaric or isochoric. Modes with $\mathbf{k
\cdot B }\neq 0$ are strongly affected by CR diffusion. When the streaming time
is shorter than the CR diffusion time, thermally unstable modes (with
$\mathbf{k \cdot B }\neq 0$) are waves propagating at a speed $\propto$ the
Alfv\'en speed. Halo gas in photoionization equilibrium is thermally stable
independent of CR pressure, while gas in collisional ionization equilibrium is
unstable for physically realistic parameters. In gravitationally stratified
plasmas, the oscillation frequency of thermally overstable modes can be higher
in the presence of CR streaming than the buoyancy/free-fall frequency. This may
modify the critical $t_{\rm cool}/t_{\rm ff}$ at which multiphase gas is
present. The criterion for convective instability of a stratified, CR-heated
medium can be written in the familiar Schwarzschild form $d s_{\rm eff} / d z <
0$, where $s_{\rm eff}$ is an effective entropy involving the gas and CR
pressures. We discuss the implications of our results for the thermal evolution
and multiphase structure of galaxy halos, groups and clusters.
