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  Forced motion near black holes

Gair, J. R., Flanagan, E. E., Drasco, S., Hinderer, T., & Babak, S. (2011). Forced motion near black holes. Physical Review D, 83(4): 044037. doi:10.1103/PhysRevD.83.044037.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-000F-1052-8 Version Permalink: http://hdl.handle.net/11858/00-001M-0000-002A-1E23-D
Genre: Journal Article

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 Creators:
Gair, Jonathan R., Author
Flanagan, Eanna E., Author
Drasco, Steve1, Author              
Hinderer, Tanja2, Author              
Babak, Stanislav1, Author              
Affiliations:
1Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_24013              
2Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290              

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Free keywords: General Relativity and Quantum Cosmology, gr-qc, Astrophysics, Galaxy Astrophysics, astro-ph.GA, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
 Abstract: We present two methods for integrating forced geodesic equations in the Kerr spacetime, which can accommodate arbitrary forces. As a test case, we compute inspirals under a simple drag force, mimicking the presence of gas. We verify that both methods give the same results for this simple force. We find that drag generally causes eccentricity to increase throughout the inspiral. This is a relativistic effect qualitatively opposite to what is seen in gravitational-radiation-driven inspirals, and similar to what is observed in hydrodynamic simulations of gaseous binaries. We provide an analytic explanation by deriving the leading order relativistic correction to the Newtonian dynamics. If observed, an increasing eccentricity would provide clear evidence that the inspiral was occurring in a non-vacuum environment. Our two methods are especially useful for evolving orbits in the adiabatic regime. Both use the method of osculating orbits, in which each point on the orbit is characterized by the parameters of the geodesic with the same instantaneous position and velocity. Both methods describe the orbit in terms of the geodesic energy, axial angular momentum, Carter constant, azimuthal phase, and two angular variables that increase monotonically and are relativistic generalizations of the eccentric anomaly. The two methods differ in their treatment of the orbital phases and the representation of the force. In one method the geodesic phase and phase constant are evolved together as a single orbital phase parameter, and the force is expressed in terms of its components on the Kinnersley orthonormal tetrad. In the second method, the phase constants of the geodesic motion are evolved separately and the force is expressed in terms of its Boyer-Lindquist components. This second approach is a generalization of earlier work by Pound and Poisson for planar forces in a Schwarzschild background.

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 Dates: 2010-12-222011-02-222011
 Publication Status: Published in print
 Pages: 28 pages, 2 figures, submitted to Phys. Rev. D; v2 has minor changes for consistency with published version, plus a new section discussing the relative advantages of the two approaches
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 Identifiers: arXiv: 1012.5111
DOI: 10.1103/PhysRevD.83.044037
URI: http://arxiv.org/abs/1012.5111
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Title: Physical Review D
  Other : Phys. Rev. D.
Source Genre: Journal
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Publ. Info: Lancaster, Pa. : Published for the American Physical Society by the American Institute of Physics
Pages: - Volume / Issue: 83 (4) Sequence Number: 044037 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: /journals/resource/111088197762258