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The asymptotic conformal invariance in Chern-Simons theory with matter in curved space-time // Tomsk State Pedagogical University Bulletin. 2004. Issue 7 (44). P. 57-59

We consider the asymptoic behaviour of the Chern - Simons (CS) theory with matter in curved space - time. The asymptotics of effective couplings are discussed.

FR W Cosmology with a Non-Linear Ingomogeneous Eq uation of State // Tomsk State Pedagogical University Bulletin. 2011. Issue 5 (107). P. 31-34

A dark Friedman-Robertson-Walker fluid governed by a non-linear ingomogeneous equation of state (EoS) is considered that it can be viewed as a conveniently simple paradigm for the whole class of models that exhibit phase transitions from a non-phantom towards a phantom era. On the other hand, such dark fluid models may also describe quintessence-like cosmic acceleration. Adding a cosmological constant-like term to the EoS led us to the conclusion that at some t = t1 a future singularity forms, in the sense that the energy density and the Hubble parameter simultaneously approach infinity at this value.

Keywords: dark energy, cosmological singularity, cosmic acceleration

Dark energy with special form inhomogeneous equation of state // Tomsk State Pedagogical University Bulletin. 2011. Issue 8 (110). P. 20-23

The four-dimensional flat Friedman universe filled with ideal fluid with a nonlinear inhomogeneous equation of state depending on time is considered. The equations of motion are solved. It is shown that in some cases there appears a quasi-periodical universe. On the other hand, such dark fluid models may also describe quintessence-like cosmic acceleration. The appearance of future singularities resulting from various choices for the input parameters is discussed.

Keywords: темная энергия, космологическая сингулярность, космическое ускорение

QUASI-RIP UNIVERSE INDUCED BY THE FLUID WITH INHOMOGENEOUS EQUATION OF STATE. // Tomsk State Pedagogical University Bulletin. 2012. Issue 13 (128). P. 42-44

We investigate a specic model for a dark energy which lead to the Quasi-Rip cosmology. In the Quasi-Rip model the equation of state parameter w is less than -1 in the rst stage, but then in the second stage is larger than -1. The conditions for the appearance the Quasi-Rip in the terms of the parameters equation of state are received.

Keywords: dark energy, cosmological constant, equation of state, bound structures