The effect of rotation on the thermal instability of stratified galactic atmospheres - II. The formation of High Velocity Clouds

Abstract

Whether High Velocity Clouds (HVCs) can form by condensation of the hot ($T\sim 10^6\mathrm{K}$) Galactic corona as a consequence of thermal instabilities has been controversial. Here we re-examine this problem and we suggest that rotation of the corona might be a missing key ingredient. We do this by studying the evolution of the models of rotating galactic coronae presented in Sormani et al. (2018) under the presence of cooling and thermal conduction. We combine a linear stability analysis with the results of local and global hydrodynamical simulations. We find that condensations are likely to occur in regions where the corona has substantial rotational support. Under reasonably general assumptions on the rotation profile of the corona, the locations where condensations are expected are in remarkable agreement with the observed location of the major non-magellanic HVCs complexes in our Galaxy (namely, at distances $<15\mathrm{kpc}$ from the Sun and within $30^{\circ }$ from the disc plane). We conclude that HVCs can form by thermal instabilities provided that (i) the corona is rotating substantially in the inner ($R<50\mathrm{kpc}$) parts, as suggested by current observational data and predicted by cosmological simulations of galaxy formation; (ii) close to the disc the corona is well-represented by a nearly-equilibrium stratified rotating structure (as opposed to a fast cooling flow). Our results also suggest that a better understanding of the disc-halo interface, including supernova feedback, is critical to understand the origin of HVCs.

Accepted for publication in MNRAS. Animations can be found at https://www.ita.uni-heidelberg.de/~mattia/download/therm/paper_II.zip

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• The role of the halo magnetic field on accretion through High-Velocity Clouds
• Clouds accreting from the IGM are not able to feed the star formation of low-redshift disc galaxies
• Inflow of low-metallicity cool gas in the halo of the Andromeda galaxy
• Understanding the Baryon Cycle: Fueling Star Formation via Inflows in Milky Way-like Galaxies
• Resolving the formation of cold HI filaments in the high velocity cloud complex C
• Predictions for the X-ray circumgalactic medium of edge-on discs and spheroids