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We characterize the Magellanic Corona model of the formation of theMagellanic Stream, which we introduced in Lucchini et al. (2020, 2021). Usinghigh-resolution hydrodynamic simulations, we constrain the properties of theprimordial Magellanic Clouds, including the Magellanic Corona -- the gaseoushalo around the Large Magellanic Cloud (LMC). With an LMC mass of$1.75\times10^{11}$ M$_\odot$, a Magellanic Corona of $>5\times10^9$ M$_\odot$at $3\times10^5$ K, a total Small Magellanic Cloud mass $<10^{10}$ M$_\odot$,and a Milky Way corona of $2\times10^{10}$ M$_\odot$, we can reproduce theobserved total mass of the neutral and ionized components of the TrailingStream, ionization fractions along the Stream, morphology of the neutral gas,and on-sky extent of the ionized gas. The inclusion of advanced physicalroutines in the simulations allow the first direct comparison of ahydrodynamical model with UV absorption-line spectroscopic data. Our modelreproduces O I, O VI, and C IV observations from HST/COS and FUSE. The strippedmaterial is also nearby ($<50$ kpc from the Sun), as found in our prior modelsincluding a Magellanic Corona.

Properties of the Magellanic Corona Model for the formation of the Magellanic Stream