Cold HI in Turbulent Eddies and Galactic Spiral Shocks

Details Cold HI in Turbulent Eddies and Galactic Spiral Shocks Cold HI in Turbulent Eddies and Galactic Spiral Shocks

2007-03-03

arxiv.org/abs/astro-ph/0703058v1

Astronomy and Astrophysics

Astrophysics

4 pages, 5 figure panels, contributed talk in IAU Symposium 237, "Triggered Star Formation in a Turbulent ISM" (eds. Elmegreen

Scientific paper

10.1017/S1743921307001731

HI 21cm-line self-absorption (HISA) reveals the shape and distribution of cold atomic clouds in the Galactic disk. Many of these clouds lack corresponding CO emission, despite being colder than purely atomic gas in equilibrium models. HISA requires background line emission at the same velocity, hence mechanisms that can produce such backgrounds. Weak, small-scale, and widespread absorption is likely to arise from turbulent eddies, while strong, large-scale absorption appears organized in cloud complexes along spiral arm shocks. In the latter, the gas may be evolving from an atomic to a molecular state prior to star formation, which would account for the incomplete HISA-CO agreement.

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