  In the inflation-based cosmology the dark matter (DM) density component
starts moving with respect to the universal expansion at $z_{\rm eq}\sim 3,200$
while baryons remain frozen until $z_{\rm rec}\sim 1,100$. It has been
suggested that in this case post-linear corrections to the evolution of small
fluctuations would result, for the standard $\Lambda$-dominated cold DM (CDM)
model, in delayed formation of early objects as supersonic advection flows
develop after recombination, so baryons are not immediately captured by the DM
gravity on small scales. We develop the hydrodynamical description of such
two-component advection and show that, in the supersonic regime, the advection
within irrotational fluids is governed by the gradient of the difference of the
kinetic energies of the two (DM and baryonic here) components. We then apply
this formalism to the case where DM is made up of LIGO-type black holes (BHs)
and show that there the advection process on scales relevant for early
structure collapse will differ significantly from the earlier discussed (CDM)
case because of the additional granulation component to the density field
produced during inflation. The advection here will lead efficiently to the
common motion of the DM and baryon components on scales relevant for collapse
and formation of first luminous sources.This leads to early collapse making
easier to explain the existence of supermassive BHs observed in quasars at high
$z>7$. The resultant net advection rate reaches minimum around $< 10^9M_\odot$
and subsequently rises to a secondary maximum near the typical mass of $\sim
10^{12}M_\odot$, which may be an important consideration for formation of
galaxies at z<(a few).
