  We studied the general advective accretion solutions around the Kerr black
hole (BH) with investigating two types of inflow gases at the outer accretion
boundary (AB). We classified these two types of gases as a \cm and a \hm inflow
gas at the outer AB on the basis of their temperatures and solutions. We found
that the \hm gas is more efficient for angular momentum transportation around
the outer AB than the \cm gas. The \hm gas can give global multiple
\cite[popular as shock solution][]{c89} or single sonic point solutions and the
\cm can give smooth global solution \cite[popular as ADAF][]{ny94} or two sonic
point solutions. These solutions also represented on a plane of energy and
angular momentum ($\be-L_0$) parameter space. Theoretically for the first time,
we explored the relation between the nature of accretion solutions with the
nature of initial accreting gas at the AB with detail computational and
possible physical analysis. We also found that the surface density of the flow
is highly affected with changing of the temperature at the AB, which can alter
the radiative emissivities of the flow. The flow variables of various advective
solutions also compared. On the basis of those results, we plotted some inner
disk structures around the BHs. Doing so, we conjectured about the
persistent/transient nature of spectral states, soft-excess and time scales of
variabilities around the black hole $X-$ ray binaries (BXBs) and active
galactic nuclei (AGNs).
