The Dynamics of Superbubbles in the Large Magellanic Cloud
Based on the stellar populations observed within this sample of LMC
superbubbles, I use a numerical version of the standard, pressure-driven
bubble model to investigate the shell dynamics. The
results fall into two distinct categories corresponding to a subset of
objects for which the observed expansion velocity is too large for the
observed shell radius (``high-velocity'' superbubbles), and a subset
of objects which appears more dynamically consistent with the model
(``low-velocity superbubbles''). Both subsets of objects imply an
overestimate in the shell growth rate equivalent to an overestimate
in input power by up to an order of magnitude.
The high-velocity objects exhibit X-ray
evidence of supernova activity, suggesting that the dynamical
discrepancy is due to acceleration by SNR impacts.
1996 ApJ, 467, 666
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