  We consider nebulae which are created around binary systems containing
rotation powered pulsars and companion stars with strong stellar winds. It is
proposed that the stellar and pulsar winds have to mix at some distance from
the binary system, defined by the orbital period of the companion stars and the
velocity of the stellar wind. The mixed pulsar-stellar wind expands with a
specific velocity determined by the pulsar power and the mass loss rate of the
companion star. Relativistic particles, either from the inner pulsar
magnetosphere and/or accelerated at the shocks between stellar and pulsar
winds, are expected to be captured and isotropized in the reference frame of
the mixed wind. Therefore, they can efficiently comptonize stellar radiation
producing GeV-TeV $\gamma$-rays in the inverse Compton process. We calculate
the $\gamma$-ray spectra expected in such scenario for the two example binary
systems: J1816+4510 which is the redback type millisecond binary and LS 5039
which is supposed to contain energetic pulsar. It is concluded that the steady
TeV $\gamma$-ray emission from J1816+4510 should be on the 100 hr sensitivity
limit of the planned Cherenkov Telescope Array, provided that $\epsilon\sim
10%$ of the rotational energy lost by the pulsar is transferred to TeV
electrons. On the other hand, the comparison of the predicted steady TeV
$\gamma$-ray emission, expected from $\gamma$-ray binary LS 5039, with the
observations of the TeV emission in a low state, reported by the H.E.S.S.
Collaboration, allows us to put stringent upper limit on the product of the
part of the hemisphere in which the mixed pulsar-stellar wind is confined,
$\Delta_{\rm mix}$, and the energy conversion efficiency, $\epsilon$, from the
supposed pulsar to the TeV electrons injected in this system, $\Delta_{\rm
mix}\cdot \epsilon <1%$.
