A Model for Line Absorption and Emission from Turbulent Mixing Layers

Abstract

Turbulent mixing layers (TMLs) are ubiquitous in multiphase gas. They can potentially explain observations of high ions such as O VI, which have significant observed column densities despite short cooling times. Previously, we showed that global mass, momentum and energy transfer between phases mediated by TMLs is not sensitive to details of thermal conduction or numerical resolution. By contrast, we show here that observables such as temperature distributions, column densities and line ratios are sensitive to such considerations. We explain the reason for this difference. We develop a prescription for applying a simple 1D conductive-cooling front model which quantitatively reproduces 3D hydrodynamic simulation results for column densities and line ratios, even when the TML has a complex fractal structure. This enables sub-grid absorption and emission line predictions in large scale simulations. The predicted line ratios are in good agreement with observations, while observed column densities require numerous mixing layers to be pierced along a line of sight.

arXiv commentAccepted for publication in MNRASL; 5 pages, 6 figures

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Cited by in corpus (5)

• The Structure of Multiphase Galactic Winds
• The CGM${}^2$ Survey: Circumgalactic O VI from dwarf to massive star-forming galaxies
• The Anatomy of a Turbulent Radiative Mixing Layer: Insights from an Analytic Model with Turbulent Conduction and Viscosity
• Radiative Turbulent Mixing Layers and the Survival of Magellanic Debris
• Absorption-based Circumgalactic Medium Line Emission Estimates