The survival of gas clouds in the circumgalactic medium of Milky Way-like galaxies

• DOI: 10.1093/mnras/stx1239
• Publication Date: 2017-05-20T07:07:43Z
• Authors: L. Armillotta; F. Fraternali; J. K. Werk; J. X. Prochaska; F. Marinacci
• Keywords: conduction; FOS: Physical sciences; Astrophysics - Astrophysics of Galaxies; 01 natural sciences; 520; COS-HALOS SURVEY; methods: numerical; galaxies: haloes; HOT GASEOUS HALO; COMPLEX-C; IONIZED-GAS; THERMAL CONDUCTION; Astrophysics of Galaxies (astro-ph.GA); hydrodynamics; 0103 physical sciences; MAGELLANIC STREAM; STAR-FORMING GALAXIES; LOW-REDSHIFT; intergalactic medium; conduction, hydrodynamics, methods: numerical, galaxies: haloes, intergalactic medium; HIGH-VELOCITY CLOUDS; GALACTIC HALO

Observational evidence shows that low-redshift galaxies are surrounded by extended haloes of multiphase gas, the so-called 'circumgalactic medium' (CGM). To study the survival of relatively cool gas (T < 10^5 K) in the CGM, we performed a set of hydrodynamical simulations of cold (T = 10^4 K) neutral gas clouds travelling through a hot (T = 2x10^6 K) and low-density (n = 10^-4 cm^-3) coronal medium, typical of Milky Way-like galaxies at large galactocentric distances (~ 50-150 kpc). We explored the effects of different initial values of relative velocity and radius of the clouds. Our simulations were performed on a two-dimensional grid with constant mesh size (2 pc) and they include radiative cooling, photoionization heating and thermal conduction. We found that for large clouds (radii larger than 250 pc) the cool gas survives for very long time (larger than 250 Myr): despite that they are partially destroyed and fragmented into smaller cloudlets during their trajectory, the total mass of cool gas decreases at very low rates. We found that thermal conduction plays a significant role: its effect is to hinder formation of hydrodynamical instabilities at the cloud-corona interface, keeping the cloud compact and therefore more difficult to destroy. The distribution of column densities extracted from our simulations are compatible with those observed for low-temperature ions (e.g. SiII and SiIII) and for high-temperature ions (OVI) once we take into account that OVI covers much more extended regions than the cool gas and, therefore, it is more likely to be detected along a generic line of sight.<br/>12 pages, 10 figures. Accepted for publication in MNRAS<br/>