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The Magellanic Stream is sculpted by its infall through the Milky Way'scircumgalactic medium, but the rates and directions of mass, momentum, andenergy exchange through the Stream-halo interface are relative unknownscritical for determining the origin and fate of the Stream. Complementary tolarge-scale simulations of LMC-SMC interactions, we apply new insights derivedfrom idealized, high-resolution "cloud-crushing" and radiative turbulent mixinglayer simulations to the Leading Arm and Trailing Stream. Contrary to classicalexpectations of fast cloud breakup, we predict that the Leading Arm and much ofthe Trailing Stream should be surviving infall and even gaining mass due tostrong radiative cooling. Provided a sufficiently supersonic tidal swing-outfrom the Clouds, the present-day Leading Arm could be a series of high-densityclumps in the cooling tail behind the progenitor cloud. We back up our analyticframework with a suite of converged wind-tunnel simulations, finding thatprevious results on cloud survival and mass growth can be extended to high Machnumber ($\mathcal{M}$) flows with a modified drag time $t_{drag} \propto 1 +\mathcal{M}$ and longer growth time. We also simulate the Trailing Stream; wefind that the growth time is long ($\sim$ Gyrs) compared to the infall time,and approximate H$\alpha$ emission is low on average ($\sim$few mR) but can beup to tens of mR in bright spots. Our findings also have broader extragalacticimplications for e.g. galactic winds, which we discuss.

Radiative Turbulent Mixing Layers and the Survival of Magellanic Debris