  The implication of small amounts of cohesion within relatively small rubble
pile asteroids is investigated with regard to their evolution under the
persistent presence of the YORP effect. We find that below a characteristic
size, which is a function of cohesive strength, density and other properties,
rubble pile asteroids can enter a "disaggregation phase" in which they are
subject to repeated fissions after which the formation of a stabilizing binary
system is not possible. Once this threshold is passed rubble pile asteroids may
be disaggregated into their constituent components within a finite time span.
These constituent components will have their own spin limits -- albeit
potentially at a much higher spin rate due to the greater strength of a
monolithic body. The implications of this prediction are discussed and include
modification of size distributions, prevalence of monolithic bodies among
meteoroids and the lifetime of small rubble pile bodies in the solar system.
The theory is then used to place constraints on the strength of binary
asteroids characterized as a function of their type.
