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We investigate the interactions of energetic hadronic particles with themedia in outflows from star-forming protogalaxies. These particles undergopion-producing interactions which can drive a heating effect in the outflow,while those advected by the outflow also transport energy beyond the galaxy,heating the circumgalactic medium. We investigate how this process evolves overthe length of the outflow and calculate the corresponding heating rates inadvection-dominated and diffusion-dominated cosmic ray transport regimes. In apurely diffusive transport scenario, we find the peak heating rate reaches$10^{-26}\;\! {\rm erg~cm}^{-3}\;\! {\rm s}^{-1}$ at the base of the outflowwhere the wind is driven by core-collapse supernovae at an event rate of 0.1$\text{yr}^{-1}$, but does not extend beyond 2 kpc. In the advection limit, thepeak heating rate is reduced to $10^{-28}\;\! {\rm erg~cm}^{-3}\;\! {\rms}^{-1}$, but its extent can reach to tens of kpc. Around 10% of the cosmicrays injected into the system can escape by advection with the outflow wind,while the remaining cosmic rays deliver an important interstellar heatingeffect. We apply our cosmic ray heating model to the recent observation of thehigh-redshift galaxy MACS1149-JD1 and show that it could account for thequenching of a previous starburst inferred from spectroscopic observations.Re-ignition of later star-formation may be caused by the presence offilamentary circumgalactic inflows which are reinstated after cosmic rayheating has subsided.

Hadronic Interactions of Energetic Charged Particles in Protogalactic Outflow Environments and Implications for the Early Evolution of Galaxies