  It is generally believed that high energy radiation (power-law components)
can be mostly produced by a hot corona gas in the accreting black holes. There
is a very popular hybrid disk radial coupling model that the inner part of cool
Keplerian disk (or Shakura-Sunyaev disk) can produce advection-dominated
accretion flow or corona-like structure, which can also generate outflows/jets.
Here we argue that this simple coupling model cannot explain the whole
hardness-intensity diagram of the spectral states and their transitions, and
associated jets of a $X-$ray binary. Based on recent theoretical works on
advective disk structures around a black hole, as well as many observational
behaviors of a source, we conclude that there should be a third component of
hot accretion flow with the radial coupling model, which can successfully
explain all the spectral states and transitions. Interestingly, this model also
provides a new scenario for the jet generation, launching, and evolution during
the states with help of created barrier of the inner flow. We have also find
out the jet kinetic power expression with our new jet generation scenario.
