Triggered Star Formation and the Dynamics of a Superbubble in the LMC: The OB Association LH 47/48 in DEM 152

Details Triggered Star Formation and the Dynamics of a Superbubble in the LMC: The OB Association LH 47/48 in DEM 152 Triggered Star Formation and the Dynamics of a Superbubble in the LMC: The OB Association LH 47/48 in DEM 152

Oct 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...452..210o&link_type=abstract

Astrophysical Journal v.452, p.210

Astronomy and Astrophysics

Astronomy

89

Galaxies: Magellanic Clouds, Galaxies: Star Clusters, Ism: Bubbles, Ism: Individual Alphanumeric: Dem 152, Stars: Formation

Scientific paper

We examine the stellar population of an OB association, LH 47/48, which is associated with a superbubble H II region, DEM 152 in the N44 nebular complex of the Large Magellanic Cloud. With C D photometry and spectroscopy of the massive stars, we find no evidence that an unusual stellar population gave rise to the shell morphology of the gas. The slope of the initial mass function, Γ = -1.3±0.2 is consistent with that of other OB associations in the LMC, and there is no significant difference in the initial mass function internal or external to the supershell The inferred stellar ionizing flux is consistent with the observed nebular Hα flux. We do find evidence for triggered star formation: the H-R diagram suggests an age of ≲ 10 Myr for the population interior to the bubble with more recent, ≲ 5 Myr, star formation on the exterior. Using the detailed data on the stellar population, we compare a numerical form of the Weaver et al. (1977) evolutionary model for wind-driven bubbles with the observed shell kinematics. We find a substantial discrepancy: the observed shell radius is too small and/or expansion velocity too large to be explained with this version of the model. We discuss possible explanations for the inconsistency.

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