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We present an analysis of new and published data on P/2013 R3, the firstasteroid detected while disintegrating. Thirteen discrete components aremeasured in the interval between UT 2013 October 01 and 2014 February 13. Wedetermine a mean, pair-wise velocity dispersion amongst these components of$\Delta v = 0.33\pm0.03$ m s$^{-1}$ and find that their separation times arestaggered over an interval of $\sim$5 months. Dust enveloping the system has,in the first observations, a cross-section $\sim$30 km$^2$ but fadesmonotonically at a rate consistent with the action of radiation pressuresweeping. The individual components exhibit comet-like morphologies and alsofade except where secondary fragmentation is accompanied by the release ofadditional dust. We find only upper limits to the radii of any embedded solidnuclei, typically $\sim$100 to 200 m (geometric albedo 0.05 assumed). Combined,the components of P/2013 R3 would form a single spherical body with radius$\lesssim$400 m, which is our best estimate of the size of the precursorobject. The observations are consistent with rotational disruption of a weak(cohesive strength $\sim$50 to 100 N m$^{-2}$) parent body, $\sim$400 m inradius. Estimated radiation (YORP) spin-up times of this parent are $\lesssim$1Myr, shorter than the collisional lifetime. If present, water ice sublimatingat as little as 10$^{-3}$ kg s$^{-1}$ could generate a torque on the parentbody rivaling the YORP torque. Under conservative assumptions about thefrequency of similar disruptions, the inferred asteroid debris production rateis $\gtrsim$10$^3$ kg s$^{-1}$, which is at least 4% of the rate needed tomaintain the Zodiacal Cloud.

Anatomy of an Asteroid Break-Up: The Case of P/2013 R3