Dynamical Chern-Simons Modified Gravity I: Spinning Black Holes in the Slow-Rotation Approximation

Details Dynamical Chern-Simons Modified Gravity I: Spinning Black Holes in the Slow-Rotation Approximation Dynamical Chern-Simons Modified Gravity I: Spinning Black Holes in the Slow-Rotation Approximation

2009-02-26

arxiv.org/abs/0902.4669v3

Phys.Rev.D79:084043,2009

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

13 pages, no figures, replaced with version accepted for publication in Phys. Rev. D. This version corrects a minor typo in Eq

Scientific paper

10.1103/PhysRevD.79.084043

The low-energy limit of string theory contains an anomaly-canceling correction to the Einstein-Hilbert action, which defines an effective theory: Chern-Simons (CS) modified gravity. The CS correction consists of the product of a scalar field with the Pontryagin density, where the former can be treated as a background field (non-dynamical formulation) or as an evolving field (dynamical formulation). Many solutions of general relativity persist in the modified theory; a notable exception is the Kerr metric, which has sparked a search for rotating black hole solutions. Here, for the first time, we find a solution describing a rotating black hole within the dynamical framework, and in the small-coupling/slow-rotation limit. The solution is axisymmetric and stationary, constituting a deformation of the Kerr metric with dipole scalar "hair," whose effect on geodesic motion is to weaken the frame-dragging effect and shift the location of the inner-most stable circular orbit outwards (inwards) relative to Kerr for co-rotating (counter-rotating) geodesics. We further show that the correction to the metric scales inversely with the fourth power of the radial distance to the black hole, suggesting it will escape any meaningful bounds from weak-field experiments. For example, using binary pulsar data we can only place an initial bound on the magnitude of the dynamical coupling constant of $\xi^{1/4} \lesssim 10^{4} {\textrm{km}}$. More stringent bounds will require observations of inherently strong-field phenomena.

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