Singularities in Graviton-Dilaton System: Their Implications on the PPN Parameters and the Cosmological Constant

dc.creatorRama, S. Kalyana
dc.date1994-11-10
dc.date1995-05-25
dc.date.accessioned2026-07-07T09:03:50Z
dc.date.available2026-07-07T09:03:50Z
dc.descriptionAlternatives to Einstein's theory of general relativity can be distinguished by measuring the parametrised post Newtonian parameters. Two such parameters $β$ and $γ$, equal to one in Einstein theory, can be obtained from static spherically symmetric solutions. For the graviton-dilaton system, as in Brans-Dicke or low energy string theory, we find that if $γ\ne 1$ for a charge neutral point star, then there exist naked singularities. Thus, if $γ$ is measured to be different from one, then it cannot be explained by these theories, without implying naked singularities. We also couple a cosmological constant $Λ$ to the graviton-dilaton system, a la string theory. We find that static spherically symmetric solutions in low energy string theory, which describe the gravitational field of a point star in the real universe atleast upto a distance $r_* \simeq {\cal O} ({\rm pc})$, always lead to curvature singularities. These singularities are stable and much worse than the naked ones. Requiring their absence upto a distance $r_*$ implies a bound $| Λ| < 10^{- 102} (\frac{r_*}{\rm pc})^{- 2}$ in natural units. If $r_* \simeq 1 {\rm Mpc}$ then $| Λ| < 10^{- 114}$, and if $r_*$ extends all the way upto the edge of the universe ($10^{28} {\rm cm}$) then $| Λ| < 10^{- 122}$ in natural units.
dc.description23 pages. Latex File, process twice. Revised version: A detailed discussion on naked singularities is added in section 3; a note and some new references added
dc.identifierhttps://arxiv.org/abs/hep-th/9411076
dc.identifierhttp://arxiv.org/abs/hep-th/9411076
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/149158
dc.subjectHigh Energy Physics - Theory
dc.subjectGeneral Relativity and Quantum Cosmology
dc.titleSingularities in Graviton-Dilaton System: Their Implications on the PPN Parameters and the Cosmological Constant
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