Abstract
A new high sensitivity radio survey of the Large Magellanic Cloud (LMC) has been undertaken at 1.4 GHz. Evidence for large-scale star-forming filaments has come from this new data. The radio results are complemented by an IRAS image of the LMC at 100 μm which shows the same large-scale filaments. Additional calculations in the frame of stochastic selfpropagating star formation models are presented. The implications for the morphology of the LMC are discussed. 1. 1.|The immediate past history of star formation and the distribution of dust in the LMC show coherent regular strings. As many as six or seven very extensive star-forming features can be recognized. 2. 2.|The optical bar of the LMC is not directly related to the star-forming pattern; it appears to reflect an earlier period in the evolution of the galaxy. 3. 3.|The stochastic selfpropagating star formation models simulate very realistically the observed distribution of young stars and molecular cloud or dust features but they do not explain the function of the 30 Doradus nebula which is also a site of a burst of star formation.
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