V. I. Dokuchaev

Black Hole Mass Decreasing due to Phantom Energy Accretion

Solution for a stationary spherically symmetric accretion of the relativistic perfect fluid with an equation of state p(rho) onto the Schwarzschild black hole is presented. This solution is a generalization of Michel solution and applicable to the problem of dark energy accretion. It is shown that accretion of phantom energy is accompanied by the gradual decrease of the black hole mass. Masses of all black holes tend to zero in the phantom energy Universe approaching the Big Rip.

Small-scale clumps in the galactic halo and dark matter annihilation

Production of small-scale DM clumps is studied in the standard cosmological scenario with an inflation-produced primeval fluctuation spectrum. Special attention is given to three following problems: (i) The mass spectrum of small-scale clumps with

Dark energy cosmology with generalized linear equation of state

M \lesssim 10^3 M_{\odot}

The accretion of dark energy onto a black hole

is calculated with tidal destruction of the clumps taken into account within the hierarchical model of clump structure. Only 0.1 - 0.5% of small clumps survive the stage of tidal destruction in each logarithmic mass interval

Destruction of small-scale dark matter clumps in the hierarchical structures and galaxies

\Delta\ln M\sim1

ULTRAHARD FLUID AND SCALAR FIELD IN THE KERR-NEWMAN METRIC

. (ii) The mass distribution of clumps has a cutoff at

Small-scale clumps of dark matter

M_{\rm min}

Remnants of dark matter clumps

due to diffusion of DM particles out of a fluctuation and free streaming at later stage.

Perfect fluid and scalar field in the Reissner-Nordstrom metric

M_{\rm min}

Superdense cosmological dark matter clumps

is a model dependent quantity. In the case the neutralino, considered as a pure bino, is a DM particle,