Horizon pretracking

Schnetter, Erik; Herrmann, Frank; Pollney, Denis

doi:10.1103/physrevd.71.044033

Cited by 18 publications

(47 citation statements)

References 31 publications

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“…Its ADM mass is M ADM 1:007 88, the initial proper horizon separation is L 4:99M ADM , and the horizons have initially the angular momentum J 0:78M 2 ADM and angular velocity 0:17=M ADM . The common apparent horizon forms at about t 17:5, which we verified through pretracking [74]. Figure 8 shows the shape of the various MOTSs at a time t 18, a short while after the common horizon has formed.…”

Section: B Nonaxisymmetric Black Hole Collisionsupporting

confidence: 61%

Introduction to dynamical horizons in numerical relativity

2006

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This paper presents a quasilocal method of studying the physics of dynamical black holes in numerical simulations. This is done within the dynamical horizon framework, which extends the earlier work on isolated horizons to time-dependent situations. In particular: (i) We locate various kinds of marginal surfaces and study their time evolution. An important ingredient is the calculation of the signature of the horizon, which can be either spacelike, timelike, or null. (ii) We generalize the calculation of the black hole mass and angular momentum, which were previously defined for axisymmetric isolated horizons to dynamical situations. (iii) We calculate the source multipole moments of the black hole which can be used to verify that the black hole settles down to a Kerr solution. (iv) We also study the fluxes of energy crossing the horizon, which describes how a black hole grows as it accretes matter and/or radiation. We describe our numerical implementation of these concepts and apply them to three specific test cases, namely, the axisymmetric head-on collision of two black holes, the axisymmetric collapse of a neutron star, and a nonaxisymmetric black hole collision with nonzero initial orbital angular momentum.

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Section: B Nonaxisymmetric Black Hole Collisionsupporting

confidence: 61%

Introduction to dynamical horizons in numerical relativity

2006

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“…For each of the MOTSs, we also look for surfaces of constant expansion [16,68] on both sides. We confirm that indeed the behavior of the apparent horizon is as expected: the expansion goes smoothly from negative to positive values as we cross the apparent horizon going outwards.…”

Section: The Various Motss For Mass Ratio 1:4mentioning

confidence: 99%

“…In numerical simulations, one typically uses marginally trapped surfaces to answer these questions. Previous numerical methods for locating marginal surfaces are described in [10][11][12][13][14][15][16]. As we shall define in more detail later, these are closed two dimensional surfaces with the topology of a sphere, in a timeslice.…”

Section: Introductionmentioning

confidence: 99%

Existence and stability of marginally trapped surfaces in black-hole spacetimes

et al. 2019

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Marginally outer trapped surfaces (MOTSs, or marginal surfaces in short) are routinely used in numerical simulations of black hole spacetimes. They are an invaluable tool for locating and characterizing black holes quasi-locally in real time while the simulation is ongoing. It is often believed that a MOTS can behave unpredictably under time evolution; an existing MOTS can disappear, and a new one can appear without any apparent reason. In this paper we show that in fact the behavior of a MOTS is perfectly predictable and its behavior is dictated by a single real parameter, the stability parameter, which can be monitored during the course of a numerical simulation. We demonstrate the utility of the stability parameter to fully understand the variety of marginal surfaces that can be present in binary black hole initial data. We also develop a new horizon finder capable of locating very highly distorted marginal surfaces and we show that even in these cases, the stability parameter perfectly predicts the existence and stability of marginal surfaces.

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“…This is based on some explicit examples such as the Vaidya spacetimes [9,10], general analytical arguments [14], numerical simulations of the collapse of a spherical scalar field [1,14] and of axi-symmetric collapse of rotating neutron stars [12,30]. From a physical and astrophysical viewpoint, it is these DHs which asymptote to the event (or, more generally, isolated) horizons in the distant future that are most interesting.…”

Section: Corollary 45 Let H Be a Regular Dh In A Spacetime (M G) Smentioning

confidence: 99%

Some uniqueness results for dynamical horizons

Ashtekar¹,

Galloway²

2005

Advances in Theoretical and Mathematical Physics

169

281

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We first show that the intrinsic, geometrical structure of a dynamical horizon (DH) is unique. A number of physically interesting constraints are then established on the location of trapped and marginally trapped surfaces in the vicinity of any DH. These restrictions are used to prove several uniqueness theorems for DH. Ramifications of some of these results to numerical simulations of black hole spacetimes are discussed. Finally, several expectations on the interplay between isometries and DHs are shown to be borne out.e-print archive: http://lanl.arXiv.org/abs/gr-qc/0503109 2 ABHAY ASHTEKAR AND GREGORY J. GALLOWAY

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Horizon pretracking

Cited by 18 publications

References 31 publications

Introduction to dynamical horizons in numerical relativity

Introduction to dynamical horizons in numerical relativity

Existence and stability of marginally trapped surfaces in black-hole spacetimes

Some uniqueness results for dynamical horizons

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