  In this paper we study Einstein-bumblebee gravity theory minimally coupled
with external matter -- a phantom/non-phantom(conventional) scalar field, find
that these scalar fields can affect the black hole solutions, i.e., giving a
hair to a black hole. In this model, the contents of the scalar field and the
forms of its potential are completely determined by the black hole spacetime.
The constant bumblebee field $b_\mu$ affects a spacetime via the coupling
constant $\ell$ and its motion equations. If $\ell>-1$, the phantom field is
admissible and the conventional scalar field is forbidden; if $\ell<-1$, the
phantom field is forbidden and the conventional scalar field is admissible.
When the bumblebee potential is quadratic, we obtain a wormhole solution
asymptotically to Ellis wormhole, it can be called Ellis-bumblebee-phantom
(EPB) wormhole which is regular everywhere and has no singularity. An
Schwarzschild-like wormhole with naked singularity and an asymptotic flat
phantom black hole solutions are also obtained. When the bumblebee potential is
linear, we derive a phantom (anti-)de-Sitter (dS/AdS) black hole solution which
can be asymptotic to Schwarzschild dS/AdS black hole. The phantom potential and
the Lagrange-multiplier $\lambda$ behave as a cosmological constant $\Lambda$.
