  There is a very popular two-zone accretion disk model that the inner part of
the non-advective Keplerian disk (Shakura-Sunyaev disk) can produce hot
advection-dominated accretion flow, which can generate high energy power-law
radiation and outflows/jets. However, we find that this simple model is
inadequate to automatically explain many properties of the sources (such as
hysteresis effect, counter-clockwise traversal in a hardness-intensity diagram,
peculiar variabilities, and association/non-association of jets in a black hole
$X-$ray binary) without considering additional assumptions. We also find some
theoretical issues in this model, such as understanding of variation of
transition region and formation of an outer disk, which has only Keplerian
distribution. Based on the recent theoretical studies on advective disk
structures, as well as, many observational behaviors of the accreting black
holes, we conclude that there should be a third component (TC) of accretion
flow parallel to the two-zone disk model, which can naturally explain all above
mentioned issues. Interestingly, this modified model also provides a new
scenario for the jet generation and evolution with the TC flow during high
energy states, which can make the jet close to the axis. We also find out an
expression of jet kinetic power.
