Cosmic-ray protons in a simulated solar-neighborhood ISM steepen from an injected p^-4.3 spectrum to p^-4.6, matching observations, with a two-zone model predicting slope gamma = (4/3)gamma_inj - 1.
Cosmic ray driven galactic winds
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abstract
Galactic winds constitute a primary feedback process in the ecology and evolution of galaxies. They are ubiquitously observed and exhibit a rich phenomenology, whose origin is actively investigated both theoretically and observationally. Cosmic rays have been widely recognized as a possible driving agent of galactic winds, especially in Milky-Way like galaxies. The formation of cosmic ray-driven winds is intimately connected with the microphysics of the cosmic ray transport in galaxies, making it an intrinsically non-linear and multiscale phenomenon. In this complex interplay the cosmic ray distribution affects the wind launching and, in turns, is shaped by the presence of winds. In this review we summarize the present knowledge of the physics of cosmic rays involved in the wind formation and of the wind hydrodynamics. We also discuss the theoretical difficulties connected with the study of cosmic ray-driven winds and possible future improvements and directions.
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Energy-Dependent Transport of Cosmic Rays in the Multiphase, Dynamic Interstellar Medium
Cosmic-ray protons in a simulated solar-neighborhood ISM steepen from an injected p^-4.3 spectrum to p^-4.6, matching observations, with a two-zone model predicting slope gamma = (4/3)gamma_inj - 1.