The Stellar Content of Superbubble H II Regions in the
Large Magellanic Cloud
M.S. Oey
I examine the stellar population enclosed within a sample of 6 LMC
superbubbles and compare these clusters with previously studied OB
associations in classical H II regions. The H-R diagrams, constructed
with spectral classifications of the most massive stars, do not reveal
any systematic differences between OB associations resident within
superbubbles and classical nebulae. The main-sequence turnoffs show
stars as massive and
luminous as those in classical H II regions, implying that the shell
formation timescale is somewhat shorter than the cluster evolutionary
timescale. The stellar winds and/or supernovae of the one or two most
massive stars must therefore dominate the formation of the superbubbles.
The star-forming events for the superbubble associations are also no
more extended in duration than that of other OB associations.
Finally, the IMF slopes are not systematically different
from those previously found. Since the OB associations within
superbubbles appear normal, the shell structures must be the result of
normal OB stellar influences. I also present a few spectrograms of
interesting massive stars, including S149, a probable new B[e]
supergiant.
1996 ApJ, 465, 231
Journal article via ADS
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