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There is a very popular two-zone accretion disk model that the inner part ofthe non-advective Keplerian disk (Shakura-Sunyaev disk) can produce hotadvection-dominated accretion flow, which can generate high energy power-lawradiation and outflows/jets. However, we find that this simple model isinadequate to automatically explain many properties of the sources (such ashysteresis 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 sometheoretical issues in this model, such as understanding of variation oftransition region and formation of an outer disk, which has only Kepleriandistribution. Based on the recent theoretical studies on advective diskstructures, as well as, many observational behaviors of the accreting blackholes, we conclude that there should be a third component (TC) of accretionflow parallel to the two-zone disk model, which can naturally explain all abovementioned issues. Interestingly, this modified model also provides a newscenario for the jet generation and evolution with the TC flow during highenergy states, which can make the jet close to the axis. We also find out anexpression of jet kinetic power.

A new prospect for jet origin and spectral state transitions with three hybrid accretion flows around black holes