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Frequent supernova explosions in compact starburst regions are a main shaperof these regions' interstellar media (ISM). In most starbursts, the supernovaremnants blast open a hot phase that fills the regions and launches asuperwind. Denser starbursts are too overpressured for hot wind formation, butsupernovae still stir up the ISM. I argue that supernovae power ubiquitousturbulence through each of the starburst ISM phases, including the hot wind,and that a fluctuation dynamo amplifies magnetic fields until they are inequipartition with the turbulence. Supernovae can drive turbulence with speedsof ~1000 km/s in the hot wind and ~20 km/s in the cold molecular gas, dependingon the outer scale. I predict magnetic field strengths of 70 muG in theGalactic Center starburst, 300 muG in M82 and NGC 253, and 2 mG in Arp 220'snuclei. The mean magnetic field strengths are a few times stronger in moleculargas than in hot winds, but do not vary strongly with density within astarburst. I explain how the dominance of supernova-driven turbulence leads tonear equipartition between the components of starburst ISM. I also considerimplications for cosmic ray (CR) diffusion in starbursts. The high amounts ofpower cascading to small scales could confine CRs very effectively instarbursts, so much that CR transport is dominated by the flow of gas ratherthan diffusion through the gas. In addition, I discuss the effects ofturbulence on X-ray line width, the far-infrared--radio correlation, observedradio polarization, and Faraday rotation measures. Finally, I discuss the manyquestions raised regarding the physics of turbulence in starbursts.

Sturm und Drang: Supernova-Driven Turbulence, Magnetic Fields, and Cosmic Rays in the Chaotic Starburst Interstellar Medium