flows onto black holes, where the existence of the inner sonic point is purely due to the presence of gravity stronger than that due to the Newtonian variety [@lt80]. It has been shown numerically as well as analytically, that such transonic matter in the multiple sonic point regime, may undergo steady or non-steady shock transition. Shock in accretion may be pressure and centrifugally supported, if the flow is rotating [@f87; @c90; @mlc94; @mrc96; @msc96; @cd04; @mgt06; @cd07; @d07; @dc08] or only be pressure supported if the flow is spherical [@co85; @ke86; @bom89]. The most popular amongst accretion disc models with advection is the so-called advection dominated accretion flow (ADAF), and it is characterized by a single sonic point close to the horizon [@nkh97]. It has been shown later, that ADAF type solution is a subset of a general viscous advective accretion solutions [@lgy99; @bdl08; @kc13]. The shock in accretion disc around black holes has been shown to exist for multispecies flows with variable adiabatic index ($\gamma$) as well [@c08; @cc11; @kscc13; @ck13].

Shock transition for accretion flow are favourable mechanism to explain many of the observational features of black hole candidates. Hot electrons in the post-shock region, abbreviated as CENBOL 