TY - JOUR

T1 - Simulating extreme-mass-ratio systems in full general relativity

AU - East, William E.

AU - Pretorius, Frans

N1 - Copyright:
Copyright 2013 Elsevier B.V., All rights reserved.

PY - 2013/5/16

Y1 - 2013/5/16

N2 - We introduce a new method for numerically evolving the full Einstein field equations in situations where the spacetime is dominated by a known background solution. The technique leverages the knowledge of the background solution to subtract off its contribution to the truncation error, thereby more efficiently achieving a desired level of accuracy. We demonstrate the method by applying it to the radial infall of a solar-type star into supermassive black holes with mass ratios ≥106. The self-gravity of the star is thus consistently modeled within the context of general relativity, and the star's interaction with the black hole computed with moderate computational cost, despite the over five orders of magnitude difference in gravitational potential (as defined by the ratio of mass to radius). We compute the tidal deformation of the star during infall, and the gravitational wave emission, finding the latter is close to the prediction of the point-particle limit.

AB - We introduce a new method for numerically evolving the full Einstein field equations in situations where the spacetime is dominated by a known background solution. The technique leverages the knowledge of the background solution to subtract off its contribution to the truncation error, thereby more efficiently achieving a desired level of accuracy. We demonstrate the method by applying it to the radial infall of a solar-type star into supermassive black holes with mass ratios ≥106. The self-gravity of the star is thus consistently modeled within the context of general relativity, and the star's interaction with the black hole computed with moderate computational cost, despite the over five orders of magnitude difference in gravitational potential (as defined by the ratio of mass to radius). We compute the tidal deformation of the star during infall, and the gravitational wave emission, finding the latter is close to the prediction of the point-particle limit.

UR - http://www.scopus.com/inward/record.url?scp=84877977045&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84877977045&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.87.101502

DO - 10.1103/PhysRevD.87.101502

M3 - Article

AN - SCOPUS:84877977045

VL - 87

JO - Physical Review D - Particles, Fields, Gravitation and Cosmology

JF - Physical Review D - Particles, Fields, Gravitation and Cosmology

SN - 1550-7998

IS - 10

M1 - 101502

ER -