  We present Newtonian three-dimensional hydrodynamical simulations of the
merger of quark stars with black holes. The initial conditions correspond to
non-spinning stars in Keplerian orbits, the code includes gravitational
radiation reaction in the quadrupole approximation for point masses. We find
that the quark star is disrupted, forming transient accretion structures around
the black hole, but 0.03 of the original stellar mass survives the initial
encounter and remains in an elongated orbit as a rapidly rotating quark
starlet, in all cases. No resolvable amount of mass is dynamically ejected
during the encounters--the black hole eventually accretes 99.99% +/- 0.01% of
the quark matter initially present.
