  In this paper we find analytical expressions for thermodynamic quantities of
scalar (tensor) and vector unparticle static black holes. We also find rotating
solutions to these systems and analyse their thermodynamics. First we consider
the static case with a spherically symmetric source for both the vector and
scalar (tensor) unparticles. We obtain thus analytical expressions to the
principal thermodynamic quantities: Hawking temperature, entropy, heat capacity
and free energy. For the scalar (tensor) case we find that the black hole
presents a residual value for the entropy when its radius goes to zero but the
other thermodynamic quantities give, for any horizon radius, a
thermodynamically unstable behavior similar to the standard black hole. For the
vector case we find a richer structure in the region in which the horizon
radius is less than the characteristic length of the unparticle theory. We
identify a phase transition and a region where the black hole can be
thermodynamically stable. Following, we show that the mentioned modifications
in the standard gravity are formally similar to those ones present in the black
holes with quintessence. With this we also show, notwithstanding, that the
unparticles cannot be a source of quintessence. By using this similarity we
find two different rotating solutions to the unparticle black holes based on
works by Ghosh and Toshmatov {\it et al}. For both cases we compute the Hawking
temperature and in the ungravity dominated regime we find, as in the static
cases, a fractalization of the event horizon. For the Gosh-like solution the
fractal dimension depends on the polar angle and on the rotation of the source.
For the Toshmatov-like one it is equal to the static case and therefore the
fractalization is not dependent on the rotation of the source.
