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Galaxies like our own, with halo masses ~1012 Msun, live in an interesting part of parameter space. Not only are they the "turnover" in the galaxy mass Schecter function, they also have the highest stellar mass (and baryon) fraction, very low bulge-to-disk ratios, and dominate the star formation of the epoch they live in. Historically, simulations of these galaxies have struggled to regulate the total stellar mass of the galaxy and produce disc-dominated systems. More recently, tensions have been identified between observations of the diffuse stellar halo and those seen in simulations. All of these effects are deeply tied to how the formation of massive stars inject energy and momentum into the galaxies which they are born in. Modelling this physics is challenging, as it involves many decades in scale across space and time, with many physical processes in play. In this talk, I will present results from a handful of recent papers that examines how we might model these processes, and how observational measurements can help us constrain our theories of how energy released by stars shapes the assembly of galaxies, their ISM, and the hot, diffuse CGM that surrounds them.