The velocity dispersion in giant extragalactic H II regions

Details The velocity dispersion in giant extragalactic H II regions The velocity dispersion in giant extragalactic H II regions

Mar 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26a....73..132d&link_type=abstract

Astronomy and Astrophysics, vol. 73, no. 1-2, Mar. 1979, p. 132-136.

Astronomy and Astrophysics

Astrophysics

42

H Ii Regions, Spiral Galaxies, Stellar Mass Ejection, Stellar Winds, B Stars, Galactic Structure, Gas Ionization, Hydrogen Ions, O Stars, Stellar Evolution, Supersonic Flow

Scientific paper

The widths of the H-alpha line profiles observed in the giant H II regions in M33 and M101 clearly show the presence of supersonic gas motions. The possibility is investigated that these motions are generated by stellar winds from the stars in the massive OB associations that must ionize these regions. The stars losing mass are assumed to have similar properties to those observed in the Galaxy. The derived models indicate that the stars with winds must be grouped spatially, with 10-100 stars driving a common shell of shocked gas. The models also show that groups of stars must have formed over the entire nebular volume on a time scale of no more than about 100,000 to 1 million yr. Thus, star formation in these regions effectively occurred simultaneously, as opposed to the sequential formation discussed for galactic H II regions.

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