Magnetized Turbulence with Cosmic Rays and Radiative Cooling*

The interstellar medium (ISM) is a magnetized and turbulent astrophysical plasma, but other components modify the characteristics of saturated magnetohydrodynamic (MHD) turbulence in the ISM. We consider two modifications: cosmic rays and radiative cooling. The emission of radiation provides a way for the ISM to lose energy. Cosmic rays, relativistic particles streaming through the ISM, can heat the ISM and drive flows. Both of these effects have individually been shown to adjust the turbulent cascade and steady state of the ISM. We examine saturated MHD turbulence modified by both cosmic rays and radiative cooling. We use the Athena++ code with a cosmic ray fluid to run turbulent box simulations. Initial simulation results will be presented illustrating the interaction of cosmic rays with a multiphase, turbulent medium. We choose to focus on cosmic rays and radiative cooling because these effects both significantly impact the formation of coherent structures in the ISM.