We present an analysis of new and published data on P/2013 R3 , the first asteroid detected while disintegrating .
Thirteen discrete components are measured in the interval between UT 2013 October 01 and 2014 February 13 .
We determine a mean , pair-wise velocity dispersion amongst these components of \Delta v = 0.33 \pm 0.03 m s ^ { -1 } and find that their separation times are staggered over an interval of \sim 5 months .
Dust enveloping the system has , in the first observations , a cross-section \sim 30 km ^ { 2 } but fades monotonically at a rate consistent with the action of radiation pressure sweeping .
The individual components exhibit comet-like morphologies and also fade except where secondary fragmentation is accompanied by the release of additional dust .
We find only upper limits to the radii of any embedded solid nuclei , 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 precursor object .
The observations are consistent with rotational disruption of a weak ( cohesive strength \sim 50 to 100 N m ^ { -2 } ) parent body , \sim 400 m in radius .
Estimated radiation ( YORP ) spin-up times of this parent are \lesssim 1 Myr , shorter than the collisional lifetime .
If present , water ice sublimating at as little as 10 ^ { -3 } kg s ^ { -1 } could generate a torque on the parent body rivaling the YORP torque .
Under conservative assumptions about the frequency of similar disruptions , the inferred asteroid debris production rate is \gtrsim 10 ^ { 3 } kg s ^ { -1 } , which is at least 4 % of the rate needed to maintain the Zodiacal Cloud .