How to move ionized gas: An introduction to the dynamics of HII regions - INSPIRE

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

William J. Henney
(
- UNAM, Inst. Astron.
)

Feb, 2006

25 pages

Published in:

Astrophys.Space Sci.Proc. 1 (2007) 103

Published: 2007

e-Print:

astro-ph/0602626 [astro-ph]

DOI:

10.1007/978-1-4020-5425-9_6

View in:

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Abstract: (arXiv)

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).

Note:

Published in the book 'Diffuse Matter from Star Forming Regions to Active Galaxies'

References(67)

Figures(0)

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