How to move ionized gas: an introduction to the dynamics of HII regions

Abstract

This review covers the dynamic processes that are important in the evolution and structure of galactic HII regions, concentrating on an elementary presentation of the physical concepts and recent numerical simulations of HII region evolution in a non-uniform medium. The contents are as follows: (1) The equations (Euler equations; Radiative transfer; Rate equations; How to avoid the dynamics; How to avoid the atomic physics). (2) Physical concepts (Static photoionization equilibrium; Ionization front propagation; Structure of a D-type front; Photoablation flows; Other ingredients - Stellar winds, Radiation pressure, Magnetic fields, Instabilities). (3) HII region evolution (Early phases: hypercompact and ultracompact regions; Later phases: compact and extended regions; Clumps and turbulence).

To be published as a chapter in 'Diffuse Matter from Star Forming Regions to Active Galaxies' - A volume Honouring John Dyson. Eds. T. W. Harquist, J. M. Pittard and S. A. E. G. Falle. 25 pages, 7 figures. Some figures degraded to meet size restriction. Full-resolution version available at http://www.ifront.org/wiki/Dyson_Festschrift_Chapter

Cited by in corpus (6)

• The Dynamics of Radiation Pressure-Dominated HII Regions
• Orion's Bar: Physical Conditions across the Definitive H+ / H0 / H2 Interface
• Radiation-magnetohydrodynamic simulations of the photoionisation of magnetised globules
• Star formation efficiency as a function of metallicity: from star clusters to galaxies
• The classical D-type expansion of spherical H II regions
• Dynamical effects of the radiative stellar feedback on the H I-to-H2 transition