Self-tuning solution of the cosmological constant problem with antisymmetric tensor field

Details Self-tuning solution of the cosmological constant problem with antisymmetric tensor field Self-tuning solution of the cosmological constant problem with antisymmetric tensor field

2001-01-04

arxiv.org/abs/hep-th/0101027v2

Nucl.Phys. B613 (2001) 306-329

Physics

High Energy Physics

High Energy Physics - Theory

LaTeX file of 21 pages, including 3 eps figues

Scientific paper

10.1016/S0550-3213(01)00397-2

We present a self-tuning solution of the cosmological constant problem with one extra dimension which is curved with a warp factor. To separate out the extra dimension and to have a self-tuning solution, a three index antisymmetric tensor field is introduced with the $1/H^2$ term in the Lagrangian. The standard model fields are located at the $y=0$ brane. The existence \cite{kklcc} of the self-tuning solution (which results without any fine tuning among parameters in the Lagrangian) is crucial to obtain a vanishing cosmological constant in a 4D effective theory. The de Sitter and anti de Sitter space solutions are possible. The de Sitter space solutions have horizons. Restricting to the spaces which contain the $y=0$ brane, the vanishing cosmological constant is chosen in the most probable universe. For this interpretaion to be valid, the existence of the self-tuning solution is crucial in view of the phase transitions. In this paper, we show explicitly a solution in case the brane tension shifts from one to another value. We also discuss the case with the $H^2$ term which leads to one-fine-tuning solutions at most.

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