Tracking Dusty Cloud Crushed by a Hot Flow

Abstract

The destruction of clouds by strong shocks and hot winds is the key process responsible for the transp orting of metals and dust from the ISM to the ICM/IGM, and establishing the multiphase structure in and around galaxies. In this work, we perform a detailed analysis of this process using two different approaches for tracking the cloud material (gas and dust): the so-called 'colored' fluid, and the Lagrangian (trace) particles. We find that for the clouds in the hot phase ($T>10^5$ K), the two methods produce significantly different mass fractions and velocities of the cloud material. In contrast, the two methods produce similar results for the clouds that are in the warm/cold phases ($T<10^5$ K). We find that the Kelvin--Helmholtz instability is suppressed in the warm clouds of size $\sim$100 pc and metallicity $Z>0.1Z_{\odot }$ due to effective gas cooling. This causes a delay in the destruction of such clouds that are interacting with the hot ICM flow. We demonstrate that the dust particles that are evacuated from their 'parent' clouds to the hot medium show different dynamics when compared to that of the Lagrangian (trace) particles. Our results indicate that the dust grains swept out to the hot gas are destroyed.

15 pages, 7 figures

References in corpus (9)

• The Dust Content of Galaxy Clusters
• Turbulent Mixing in the Interstellar Medium -- an application for Lagrangian Tracer Particles
• On the dust content of galaxy clusters
• Searching for dust in the intracluster medium from reddening of background galaxies
• Numerical comparison of Riemann solvers for astrophysical hydrodynamics
• How radiation affects superbubbles: Through momentum injection in early phase and photo-heating thereafter
• Dust in the outskirts of M31 and M33
• Dust in clusters: separating the contribution of galaxies and intracluster media
• Dust in Clusters of Galaxies