  Observed planetary debris in white dwarf atmospheres predominately originate
from the destruction of small bodies on highly eccentric ($>0.99$) orbits.
Despite their importance, these minor planets have coupled physical and orbital
evolution which has remained largely unexplored. Here, we present a novel
approach for estimating the influence of fast chaotic rotation on the orbital
evolution of high-eccentricity triaxial asteroids, and formally characterize
the propagation of their angular rotation velocities and orbital elements as
random time processes. By employing the impulse approximation, we demonstrate
that the violent gravitational interactions during periastron passages transfer
energy between the orbit and asteroid's rotation. If the distribution of spin
impulses were symmetric around zero, then the net result would be a secular
decrease of the semimajor axis and a further increase of the eccentricity. We
find evidence, however, that the chaotic rotation may be self-regulated in such
a manner that these effects are reduced or nullified. We discover that
asteroids on highly eccentric orbits can break themselves apart --- in a type
of YORP-less rotational fission --- without actually entering the Roche radius,
with potentially significant consequences for the distribution of debris and
energy requirements for gravitational scattering in metal-polluted white dwarf
planetary systems. This mechanism provides a steady stream of material
impacting a white dwarf without rapidly depleting the number of small bodies in
the stellar system.
