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Slowly rotating black holes in dynamical Chern-Simons gravity: Deformation quadratic in the spin

Kent Yagi1,*, Nicolás Yunes1, and Takahiro Tanaka2

  • 1Department of Physics, Montana State University, Bozeman, Montana 59717, USA
  • 2Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto, 606-8502, Japan

  • *kyagi@physics.montana.edu
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Phys. Rev. D 86, 044037 – Published 21 August, 2012

DOI: https://doi.org/10.1103/PhysRevD.86.044037

Abstract

We derive a stationary and axisymmetric black hole solution to quadratic order in the spin angular momentum. The previously found, linear-in-spin terms modify the odd-parity sector of the metric, while the new corrections appear in the even-parity sector. These corrections modify the quadrupole moment, as well as the (coordinate-dependent) location of the event horizon and the ergoregion. Although the linear-in-spin metric is of Petrov type D, the quadratic-order terms render it of type I. The metric does not possess a second-order Killing tensor or a Carter-like constant. The new metric does not possess closed timelike curves or spacetime regions that violate causality outside of the event horizon. The new, even-parity modifications to the Kerr metric decay less rapidly at spatial infinity than the leading order in spin, odd-parity ones, and thus, the former are more important when considering black holes that are rotating moderately fast. We calculate the modifications to the Hamiltonian, binding energy and Kepler’s third law. These modifications are crucial for the construction of gravitational wave templates for black hole binaries, which will enter at second post-Newtonian order, just like dissipative modifications found previously.

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Phys. Rev. D 86, 044037– Published 21 August, 2012
  • Received 26 June 2012
Article part of CHORUS

© 2012 American Physical Society

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