increasing number of clumps, maybe tens or hundreds at the present time. A more accurate description would involve a statistical hierarchy of effective clump sizes. This could account for both the gradient increase and the short-term fluctuations in the observed flux density. Both radio and optical evidence (e.g. Spyromilio, Stathakis & Meurer 1993, van Dyk et al. 1994, Spyromilio 1994) point to a clumpy circumstellar medium around other supernovae.

9 GHz Imaging Observations of SNR 1987A
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Resolved Radio Images of SNR 1987A
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In previous papers we have shown that the ATCA’s diffraction-limited resolution at 9 GHz of 09 is sufficient to resolve the radio emission from SNR 1987A (Staveley-Smith et al. 1993b) and that super-resolution techniques can be used to improve the resolution to $\sim0\farcs5$. At this resolution, the radio emission forms a limb-brightened shell, with brightness enhancements on the eastern and western sides (Staveley-Smith et al. 1993a; Briggs 1994; Gaensler et al. 1997).

We have continued to make regular observations of SNR 1987A at 9 GHz; observing parameters for all imaging observations are given in Table \[tab\_9ghz\]. We have analysed these data in the same manner as described by Gaensler et al. (1997), forming an image at 