Orateur
Description
GeV cosmic rays, accelerated in supernova explosions, represent a significant energetic component of the interstellar medium. Through their coupling to magnetic fields, their ability to efficiently diffuse along field lines, and their long radiative loss timescales, they provide a non-thermal feedback capable of significantly influencing galaxy evolution. In particular, they can alter the properties of large-scale galactic winds and contribute to regulating the dense gas that forms stars. Magnetohydrodynamical simulations including cosmic ray transport have highlighted the potentially key role of this non-thermal component in galaxy self-regulation. However, significant uncertainties remain, especially regarding the cosmic ray diffusion in the interstellar medium, a poorly constrained parameter that critically determines their feedback efficiency over galactic scales. In this talk, I will review recent developments and results from galaxy simulations including cosmic rays, with a focus on modeling challenges and current uncertainties.