Horizon boundary condition for black hole spacetimes

Anninos, Peter; Daues, Greg; Massó, Joan; Seidel, Edward; Suen, Wai-Mo

doi:10.1103/physrevd.51.5562

Cited by 73 publications

(142 citation statements)

References 14 publications

(37 reference statements)

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“…Nevertheless, these and similar gauge conditions have proven useful for studies of single-black-hole spacetimes [43,49]. Furthermore, if imposed only at one point, they can be used as boundary conditions on more general elliptic gauge choices, described below.…”

Section: Algebraic Conditionsmentioning

confidence: 99%

Black hole evolution by spectral methods

et al. 2000

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Current methods of evolving a spacetime containing one or more black holes are plagued by instabilities that prohibit long-term evolution. Some of these instabilities may be due to the numerical method used, traditionally finite differencing. In this paper, we explore the use of a pseudospectral collocation (PSC) method for the evolution of a spherically symmetric black hole spacetime in one dimension using a hyperbolic formulation of Einstein's equations. We demonstrate that our PSC method is able to evolve a spherically symmetric black hole spacetime forever without enforcing constraints, even if we add dynamics via a Klein-Gordon scalar field. We find that, in contrast to finite-differencing methods, black hole excision is a trivial operation using PSC applied to a hyperbolic formulation of Einstein's equations. We discuss the extension of this method to three spatial dimensions.04.25.Dm, 02.70.Hm

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Section: Algebraic Conditionsmentioning

confidence: 99%

Black hole evolution by spectral methods

et al. 2000

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“…On the other hand, certain numerical methods such as excision boundaries [3,4] use the apparent horizon to identify the region within the black hole. Knowing the common horizon location also makes it possible to adjust the dynamics of the spacetime via so-called "horizon-locking" gauges [5,6], as well as gauges which attempt to control the location of the black hole [7]. At late times, the shape and oscillations of the apparent horizon is an effective indicator of the angular momentum of the final black hole, and has been related to its quasi-normal mode ringing [8].…”

Section: Motivationmentioning

confidence: 99%

Horizon pretracking

2005

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We introduce horizon pretracking as a method for analysing numerically generated spacetimes of merging black holes. Pretracking consists of following certain modified constant expansion surfaces during a simulation before a common apparent horizon has formed. The tracked surfaces exist at all times, and are defined so as to include the common apparent horizon if it exists. The method provides a way for finding this common apparent horizon in an efficient and reliable manner at the earliest possible time. We can distinguish inner and outer horizons by examining the distortion of the surface. Properties of the pretracking surface such as its expansion, location, shape, area, and angular momentum can also be used to predict when a common apparent horizon will appear, and its characteristics. The latter could also be used to feed back into the simulation by adapting e.g. boundary or gauge conditions even before the common apparent horizon has formed.

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“…This idea is not new (see, for instance, Ref. [56]) and amounts to correcting the Gamma-driver shift condition (6) with an additional term which reflects a coordinate acceleration towards the black hole. This is most conveniently done by modeling the changes as those experienced by a damped harmonic oscillator [57].…”

Section: Fig 4 2-norm Of the Hamiltonian Constraint Along The X-axismentioning

confidence: 99%

Numerical evolutions of a black hole-neutron star system in full general relativity: Head-on collision

Löffler

Rezzolla²,

Ansorg³

2006

Phys. Rev. D

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We present the first simulations in full general relativity of the head-on collision between a neutron star and a black hole of comparable mass. These simulations are performed through the solution of the Einstein equations combined with an accurate solution of the relativistic hydrodynamics equations via high-resolution shock-capturing techniques. The initial data is obtained by following the YorkLichnerowicz conformal decomposition with the assumption of time symmetry. Unlike other relativistic studies of such systems, no limitation is set for the mass ratio between the black hole and the neutron star, nor on the position of the black hole, whose apparent horizon is entirely contained within the computational domain. The latter extends over 400M and is covered with six levels of fixed mesh refinement. Concentrating on a prototypical binary system with mass ratio 6, we find that although a tidal deformation is evident the neutron star is accreted promptly and entirely into the black hole. While the collision is completed before 300M, the evolution is carried over up to 1700M, thus providing time for the extraction of the gravitational-wave signal produced and allowing for a first estimate of the radiative efficiency of processes of this type.

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Horizon boundary condition for black hole spacetimes

Cited by 73 publications

References 14 publications

Black hole evolution by spectral methods

Black hole evolution by spectral methods

Horizon pretracking

Numerical evolutions of a black hole-neutron star system in full general relativity: Head-on collision

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