Other
Scientific paper
Oct 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989pazh...15..897s&link_type=abstract
Pis'ma v Astronomicheskii Zhurnal (ISSN 0320-0108), vol. 15, Oct. 1989, p. 897-909. In Russian. In Russian. In Russian.
Other
1
Giant Stars, Interstellar Gas, Milky Way Galaxy, Star Formation, H I Regions, H Ii Regions, Molecular Clouds, Sagittarius Constellation, Spatial Distribution, Water Masers
Scientific paper
A gradient of star group ages (0.3 to 1.2 x 10 to the 7th years) in seven large-scale (300 to 700 pc) star-gas complexes (SGCs) distinguished by Efremov and Sitnik (1988) within 0.5 to 3 kpc of the sun is found. In three SGCs of the Sagittarius-Carina arm clusters of early spectral types, young OB-associations, molecular clouds, H II regions, and young H2O masers are localized near the inner border of the arm, whereas old star groups are closer to the outer one. The age gradient observed across the Sagittarius-Carina arm gives evidence for its formation by a spiral density wave. The Cygnus arm may be near the corotation axis, since the age variation in it occurs not across but along the arm. A 'reverse' age gradient in one of the SGCs of the Perseus-Cassiopeia arm cannot be ruled out. In neighboring SGCs the direction of propagation of star formation may be different: in every complex the birth of stars begins at one edge of a giant H I cloud and propagates toward the other. Giant molecular clouds of more than 100,000 solar masses are observed mainly in regions of associations not older than 6.5 million years.
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