Abstract
A systematic study of the X-ray properties of OB associations in the Large Magellanic Cloud has been carried out using data from the Einstein Observatory. An excess of young, X-ray-bright supernova remnants is found in the vicinity of the associations. In addition, diffuse X-ray emission is detected from over two dozen other associations; luminosities in the 0.16-3.5 keV band range from 2 x 10 to the 34th (the detection threshold) to 10 to the 36th ergs/s. For several of the more luminous examples, it is shown that emission from interstellar bubbles created by the OB stellar winds alone is insufficient to explain the emission. It is concluded that transient heating of the bubble cavities by recent supernovae may be required to explain the observed X-rays and that such a scenario is consistent with the number of X-ray-bright associations and the expected supernova rate from the young stars they contain.
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