We suggest the SO(1, 1) scalar field model of dark energy. In this model, the Lagrangian may be decomposed as that of the real quintessence model and the negative coupling energy term of Φ to a. The existence of the coupling term L c leads to a wider range of w Φ and overcomes the problem of negative kinetic energy in the phantom universe model. We propose a power-law expansion kinetics model of univese with time-dependent power, which can describe the universe transition from ordinary acceleration to super acceleration. We give also a simple discussion of Big Rip singularity, and point out the possibility that the universe driven by phantom avoid it.PACS number(s) 98.80.Cq, 98.80.Hm
We calculate the local energy and the energy density of the Reisner-Norström-anti-de-Sitter black hole, study the first law of thermodynamics and show the Smarr formula for the Born-Infeld-anti-de-Sitter black hole. Applying the first law of thermodynamics to the black hole region, we analyse the three energy exchange processes between the black hole region and the outer and the inner regions.
The first law of thermodynamics for the three horizons of Reissner-Nordström quintessence (RNQ) spacetime is obtained. For a general process of RNQ spacetime, the expressions for the radius changes of the three horizons are derived. When only mass changes, the heat fluxes through the three horizons are equivalent and no heat is left in the black hole region. Finally, a further discussion on the thermal properties of an RNQ black hole is given.
We discuss the five-dimensional axisymmetric metric with
non-zero parameter η, the field equation is reduced
to the Ernst equation with
η and the Laplace equation. For η = 1, the corresponding
solution describes the five-dimensional axisymmetric spacetime
with an electrostatic field. We find that the TS solutions
can be generalized to those with arbitrary non-zero η.
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