The Survival of Multiphase Dusty Clouds in Hot Winds

Abstract

Much progress has been made recently in the acceleration of $\sim 10^4$\,K clouds to explain absorption-line measurements of the circumgalactic medium and the warm, atomic phase of galactic winds. However, the origin of the cold, molecular phase in galactic winds has received relatively little theoretical attention. Studies of the survival of $\sim 10^4$\,K clouds suggest efficient radiative cooling may enable the survival of expelled material from galactic disks. Alternatively, gas colder than 10${}^4$\,K may form within the outflow, including molecules if dust survives the acceleration process. We explore the survival of dusty clouds in a hot wind with three-dimensional hydrodynamic simulations including radiative cooling and dust modeled as tracer particles. We find that cold $\sim 10^3$\,K gas can be destroyed, survive, or transformed entirely to $\sim 10^4$K gas. We establish analytic criteria distinguishing these three outcomes which compare characteristic cooling times to the system's `cloud crushing' time. In contrast to typically studied $\sim 10^4$\,K clouds, colder clouds are entrained faster than the drag time as a result of efficient mixing. We find that while dust can in principle survive embedded in the accelerated clouds, the survival fraction depends critically on the time dust spends in the hot phase and on the effective threshold temperature for destruction. We discuss our results in the context of polluting the circumgalactic medium with dust and metals, as well as understanding observations suggesting rapid acceleration of molecular galactic winds and ram pressure stripped tails of jellyfish galaxies.

18 pages, 12 figures + Appendices. Accepted for publication in MNRAS

References in corpus (33)

• Giant Gamma-ray Bubbles from Fermi-LAT: AGN Activity or Bipolar Galactic Wind?
• A New Calculation of the Ionizing Background Spectrum and the Effects of HeII Reionization
• Draping of Cluster Magnetic Fields over Bullets and Bubbles -- Morphology and Dynamic Effects
• Star formation in a galactic outflow
• Magnetized Gas Clouds can Survive Acceleration by a Hot Wind
• The Launching of Cold Clouds by Galaxy Outflows I: Hydrodynamic Interactions with Radiative Cooling
• The strong transformation of spiral galaxies infalling into massive clusters at z~0.2
• Iron line and diffuse hard X-ray emission from the starburst galaxy M82
• The dust mass in Cassiopeia A from a spatially resolved Herschel analysis
• Efficiency of gas cooling and accretion at the disc-corona interface
• An Exact Integration Scheme for Radiative Cooling in Hydrodynamical Simulations
• Dense Molecular Gas Tracers in the Outflow of the Starburst Galaxy NGC 253
• Cosmic ray-driven galactic winds: streaming or diffusion?
• A Review of Recent Observations of Galactic Winds Driven by Star Formation
• The effect of ram pressure on the molecular gas of galaxies: three case studies in the Virgo cluster
• Dust masses for SN 1980K, SN1993J and Cassiopeia A from red-blue emission line asymmetries
• It's Cloud's Illusions I Recall: Mixing Drives the Acceleration of Clouds from Ram Pressure Stripped Galaxies
• Cold gas in the Milky Way's nuclear wind
• GASP. XV. A MUSE View of Extreme Ram-Pressure Stripping along the Line of Sight: Physical properties of the Jellyfish Galaxy JO201
• Filament formation in wind-cloud interactions. II. Clouds with turbulent density, velocity, and magnetic fields
• The Journey Counts: The Importance of Including Orbits when Simulating Ram Pressure Stripping
• Highly ordered magnetic fields in the tail of the jellyfish galaxy JO206
• On the dynamics and survival of fractal clouds in galactic winds
• AGN-stimulated Cooling of Hot Gas in Elliptical Galaxies
• The Production of Cold Gas Within Galaxy Outflows
• On the Formation of Molecular Clumps in QSO Outflows
• The mass, location and heating of the dust in the Cassiopeia A supernova remnant
• Observation of Acceleration of HI Clouds Within the Fermi Bubbles
• Revisiting the dust destruction efficiency of supernovae
• Molecular gas distribution perpendicular to the Galactic plane
• Molecular gas in the outflow of the Small Magellanic Cloud
• Thermal instability revisited
• Interactions of a shock with a molecular cloud at various stages of its evolution due to thermal instability and gravity

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