  We propose a new model of Fast Radio Bursts (FRBs) based on stellar mass
black hole-massive star binaries. We argue that the inhomogeneity of the
circumstellar materials or/and the time varying wind activities of the stellar
companion will cause the black hole to accrete at a transient super-Eddington
rate. The collision among the clumpy ejecta in the resulted jet could trigger
plasma instability. As a result, the plasma in the jet will emit coherent
curvature radiation. When the jet cone aims toward the observer, the apparent
luminosity can be $10^{41}-10^{42}$\,erg/s. The duration of the resulted flare
is $\sim$ millisecond. The high event rate of the observed non-repeating FRBs
can be explained. A similar scenario in the vicinity of a supermassive black
hole can be used to explain the interval distribution of the repeating source
FRB121102 qualitatively.
