  We report observations of the recurrent nova RS Oph using long-baseline
near-IR interferometry. We are able to resolve emission from the nova for
several weeks after the February 2006 outburst. The near-IR source initially
expands to a size of approximately 5 milli-arcseconds. However, beginning
around day 10 the IR source appears to begin to shrink, reaching approximately
2 milli-arcseconds by day 100. We combine our measured angular diameters with
previously available interferometric and photometric data to derive an emission
measure for the source, and hence are able to determine the mass-loss rate of
the nova in the days following the outburst.
