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

Löffler, Frank; Rezzolla, Luciano; Ansorg, Marcus

doi:10.1103/physrevd.74.104018

Cited by 78 publications

(74 citation statements)

References 65 publications

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“…In this way, we avoid using a moving excision boundary for the hydrodynamical variables as in [67]. From the point of view of the evolution it is safe to do this, as the evolution of the hydrodynamics inside the horizon cannot influence the evolution outside the horizon.…”

Section: Initial Data and Setupmentioning

confidence: 99%

Numerical relativity simulations of thick accretion disks around tilted Kerr black holes

et al. 2016

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In this work we present 3D numerical relativity simulations of thick accretion disks around tilted Kerr black holes. We investigate the evolution of three different initial disk models with a range of initial black hole spin magnitudes and tilt angles. For all the disk-to-black hole mass ratios considered (0.044 − 0.16) we observe significant black hole precession and nutation during the evolution. This indicates that for such mass ratios, neglecting the self-gravity of the disks by evolving them in a fixed background black hole spacetime is not justified. We find that the two more massive models are unstable against the Papaloizou-Pringle (PP) instability and that those PP-unstable models remain unstable for all initial spins and tilt angles considered, showing that the development of the instability is a very robust feature of such PP-unstable disks. Our lightest model, which is the most astrophysically favorable outcome of mergers of binary compact objects, is stable. The tilt between the black hole spin and the disk is strongly modulated during the growth of the PP instability, causing a partial global realignment of black hole spin and disk angular momentum in the most massive model with constant specific angular momentum l. For the model with non-constant lprofile we observe a long-lived m = 1 non-axisymmetric structure which shows strong oscillations of the tilt angle in the inner regions of the disk. This effect might be connected to the development of Kozai-Lidov oscillations. Our simulations also confirm earlier findings that the development of the PP instability causes the long-term emission of large amplitude gravitational waves, predominantly for the l = m = 2 multipole mode. The imprint of the BH precession on the gravitational waves from tilted BH-torus systems remains an interesting open issue that would require significantly longer simulations than those presented in this work.

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Section: Initial Data and Setupmentioning

confidence: 99%

Numerical relativity simulations of thick accretion disks around tilted Kerr black holes

et al. 2016

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“…Several gravitational wave detectors [1][2][3] have now achieved a high enough level of sensitivity that the first astrophysical observations are expected to occur within the next few years. The numerical relativity community has also matured to the point that several groups are now computing model gravitational waveforms for the inspiral and merger of black hole and neutron star binary systems [4][5][6][7][8][9][10][11][12][13]. Beyond the pioneering work of Mark Miller [14] and Stephen Fairhurst [15], however, little effort has gone into thinking about the question of how accurate these model waveforms need to be.…”

Section: Introductionmentioning

confidence: 99%

Model waveform accuracy standards for gravitational wave data analysis

2008

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Model waveforms are used in gravitational wave data analysis to detect and then to measure the properties of a source by matching the model waveforms to the signal from a detector. This paper derives accuracy standards for model waveforms which are sufficient to ensure that these data analysis applications are capable of extracting the full scientific content of the data, but without demanding excessive accuracy that would place undue burdens on the model waveform simulation community. These accuracy standards are intended primarily for broadband model waveforms produced by numerical simulations, but the standards are quite general and apply equally to such waveforms produced by analytical or hybrid analytical-numerical methods.

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“…To date, work on black hole-neutron star binaries has been limited to a few cases [19,20,21]. As a result, our understanding of this type of system is still in its infancy.…”

Section: Introductionmentioning

confidence: 99%

Simulating binary neutron stars: Dynamics and gravitational waves

et al. 2008

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We model two mergers of orbiting binary neutron stars, the first forming a black hole and the second a differentially rotating neutron star. We extract gravitational waveforms in the wave zone. Comparisons to a post-Newtonian analysis allow us to compute the orbital kinematics, including trajectories and orbital eccentricities. We verify our code by evolving single stars and extracting radial perturbative modes, which compare very well to results from perturbation theory. The Einstein equations are solved in a first order reduction of the generalized harmonic formulation, and the fluid equations are solved using a modified convex essentially non-oscillatory method. All calculations are done in three spatial dimensions without symmetry assumptions. We use the had computational infrastructure for distributed adaptive mesh refinement.

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

Cited by 78 publications

References 65 publications

Numerical relativity simulations of thick accretion disks around tilted Kerr black holes

Numerical relativity simulations of thick accretion disks around tilted Kerr black holes

Model waveform accuracy standards for gravitational wave data analysis

Simulating binary neutron stars: Dynamics and gravitational waves

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