Caratterizziamo il caldo mezzo circumgalattico (CGM) of a dwarf galaxy pair
with properties similar to the Magellanic Clouds in the \textsc{Estia}
simulazioni cosmologiche. Il sistema è costituito da un enorme nano ($M_{\cmq ciao}
\sim 10^{11.5} M_{\odot}$) e un compagno di massa inferiore ($M_{\cmq ciao} \sim
10^{10} M_{\odot}$), dynamically evolving in isolation before infall into a
Milky Way-mass halo. The massive dwarf hosts a warm coronal gas envelope with a
temperature of $T \sim 3 \times 10^5$ K, consistent with expectations for
virialized CGM in dwarf halos. Tidal interactions produce a neutral gas stream
that extends over $\sim 150$ kpc, with an \ion{H}{1} mass of $M_{\rm HI} \sim
10^8 M_{\odot}$, similar to the Magellanic Stream. Inoltre, in the
\textsc{Estia} simulation suite, we find that coronal gas is ubiquitous in all
halos with $M_{\cmq ciao} > 10^{11} M_{\odot}$, implying that massive dwarfs
generically develop extended gaseous envelopes prior to accretion. This result
has significant implications for the survival of neutral tidal structures, E
suggests that current and future high-ion UV absorption-line observations are
indicative of warm coronae surrounding LMC-mass dwarfs, independent of their
environment.

Questo articolo esplora i giri e le loro implicazioni.

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