  Given the compositional diversity of asteroids, and their distribution in
space, it is impossible to consider returning samples from each one to
establish their origin. However, the velocity and molecular composition of
primary minerals, hydrated silicates, and organic materials can be determined
by in situ dust detector instruments. Such instruments could sample the cloud
of micrometer-scale particles shed by asteroids to provide direct links to
known meteorite groups without returning the samples to terrestrial
laboratories. We extend models of the measured lunar dust cloud from LADEE to
show that the abundance of detectable impact-generated microsamples around
asteroids is a function of the parent body radius, heliocentric distance, flyby
distance, and speed. We use monte carlo modeling to show that several tens to
hundreds of particles, if randomly ejected and detected during a flyby, would
be a sufficient number to classify the parent body as an ordinary chondrite,
basaltic achondrite, or other class of meteorite. Encountering and measuring
microsamples shed from near-earth and main-belt asteroids, coupled with
complementary imaging and multispectral measurements, could accomplish a
thorough characterization of small, airless bodies.
