  The problem of the energy-momentum conservation for matter in the
gravitational field is discussed on the example of the effective gravity, which
arises in superfluids. The "gravitational" field experienced by the
relativistic-like massless quasiparticles which form the "matter" (phonons in
superfluid 4He and low-energy fermions in superfluid 3He-A), is induced by the
flow of the superfluid "vacuum". It appears that the energy-momentum
conservation law for quasiparticles, has the covariant form
T^{\mu}_{\nu;\mu}=0. "Pseudotensor" of the energy-momentum for the
"gravitational field" (superfluid condensate) appears to depend on "matter". In
the presence of the stationary "gravitational" (superfluid) field the real
thermodynamic temperature T is constant in the true dissipationless equilibrium
state with no entropy production, while the "relativistic" temperature
T/\sqrt{g_{00}} is space dependent in agreement with Tolman's law. In the
presence of the event horizon the true dissipationless equilibrium state does
not exist. The quasiequilibrium dissipative motion across the horizon is
considered. The inflationary stage of the expansion of the Universe can be
modelled using the expanding Bose-condendsate.
