Physical properties of H II regions in the Small Magellanic Cloud

Details Physical properties of H II regions in the Small Magellanic Cloud Physical properties of H II regions in the Small Magellanic Cloud

Mar 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...229..533c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 229, no. 2, March 1990, p. 533-539. Research supported by CNPq.

Physics

8

H Ii Regions, Interstellar Matter, Magellanic Clouds, Star Formation, Stellar Physics, Electron Density (Concentration), H Beta Line, Ionized Gases, Lyman Beta Radiation, Physical Properties

Scientific paper

Some physical properties of the H II regions and their ionizing stellar associations, such as the Lyman continuum photon flux, the rms electron density, and the mass of ionized gas, were derived for 30 H II regions in the SMC. Bright H II regions are found to be large and diffuse, whereas faint ones are compact; i.e., small and dense. The decrease of W(H-beta) with the increase of the nebular size and decrease of rms electron density is consistent with a trend in the sense of an H II region expansion with aging. However, the rms electron density tends to be a decreasing function of the nebular ionizing flux, which is inconsistent with a single evolutionary sequence for the H II regions.

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