Resolved shocks in clumpy media

Abstract

We study the structure of shocks in clumpy media, using a multifluid formalism. As expected, shocks broaden as they weaken: for sufficiently weak shocks, no viscous subshock appears in the structure. This has significant implications for the survival of dense clouds in regions overrun by shocks in a wide range of astrophysical circumstances, from planetary nebulae to the nuclei of starburst galaxies.

9 pages, 4 figures, Latex, MN macros, in press with MNRAS

References in corpus (4)

• Starburst-driven galactic winds: I. Energetics and intrinsic X-ray emission
• Shocked H2 and Fe+ Dynamics in the Orion Bullets
• Symbiotic starburst-black hole AGN -- I. Isothermal hydrodynamics of the mass-loaded ISM
• Self-similar evolution of wind-blown bubbles with mass loading by hydrodynamic ablation

Cited by in corpus (8)

• Galactic Winds
• The Enrichment of the Intergalactic Medium with Adiabatic Feedback I: Metal Cooling and Metal Diffusion
• The Large-scale Bipolar Wind in the Galactic Center
• The Dynamical Evolution of the Circumstellar Gas around Low- and Intermediate-Mass stars.II. The Planetary Nebula formation
• Numerical simulations of shocks encountering clumpy regions
• The Collimated Wind in NGC 253
• Numerical Simulations of a Shock Interacting with Multiple Magnetized Clouds
• Mass-Loaded Flows