Static spacetimes haunted by a phantom scalar field II: dilatonic charged solutions

Abstract

We present a method to generate static solutions in the Einstein-Maxwell system with a (phantom) dilaton field in $n(\ge 4)$-dimensions, based upon the symmetry of the target space for the nonlinear sigma model. Unlike the conventional Einstein-Maxwell-dilaton system, there appears a critical value of the coupling constant for a phantom dilaton field. In the noncritical case, the target space is $\mathbb{R}\times \mathrm{SL}(2,\mathbb{R})/H$ with the maximal subgroup $H=\{\mathrm{SO}(2),\mathrm{SO}(1,1)\}$, whereas in the critical case the target space becomes a symmetric pp-wave and the corresponding Killing vectors form a non-semisimple algebra. In either case, we apply the formalism to charge up the neutral solutions and show the analytical expression for dilatonic charged versions of (i) the Fisher solution, (ii) the Gibbons solution, and (iii) the Ellis-Bronnikov solution. We discuss global structures of these solutions in detail. It turns out that some solutions contained in the Fisher and Gibbons classes possess the parallelly propagated (p.p) curvature singularities in the parameter region where all the scalar curvature invariants remain bounded. These p.p curvature singularities are not veiled by a horizon, thrusting them into physically untenable nakedly singular spacetimes. We also demonstrate that the dilatonic-charged Ellis-Bronnikov solution admits a parameter range under which the solution represents a regular wormhole spacetime in the two-sided asymptotically flat regions.

2 figures, 1 table, 33 pages; v2: refs added, to appear in PRD

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Cited by in corpus (9)

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• Static spacetimes haunted by a phantom scalar field III: asymptotically (A)dS solutions
• Wormhole $C$ metric
• Charged Dilatonic Spacetimes in String Theory
• Classification of static black holes in Einstein phantom/dilaton Maxwell/anti-Maxwell gravity systems
• Multi-Sheet Wormholes in the Gravitational Soliton Formalism
• Robinson-Trautman solutions with scalar hair and Ricci flow
• Deflection in higher dimensional spacetime and asymptotically non-flat spacetimes