The Kozai-Lidov Mechanism in Hydrodynamical Disks

Martin, Rebecca G.; Nixon, Chris; Lubow, Stephen H.; Armitage, Philip J.; Price, Daniel J.; Doğan, S.; King, Andrew

doi:10.1088/2041-8205/792/2/l33

Cited by 157 publications

(152 citation statements)

References 49 publications

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“…The Kozai-Lidov mechanism induces antiphase oscillations in the orbital inclination and eccentricity of particles highly inclined to a binary companion (Kozai, 1962Lidov, 1962. Martin et al (2014) are the first to show that this process also occurs in a fluid disc. In our 60…”

Section: Fig 1 Shows the Simulation With An Initial Inclination Of 10mentioning

confidence: 90%

“…The accretion rate is in code units of binary mass per binary dynamical time, and the time axis is in units of the binary dynamical time where a full orbit of the binary is 2π. Martin et al (2014) were the first to show that this behaviour occurs more generally for extended discs, and is therefore probably important in many astrophysical scenarios. The increase in accretion rate for the broken discs here is only a factor of a few, rather than the orders of magnitude found in Nixon et al (2013).…”

Section: Fig 1 Shows the Simulation With An Initial Inclination Of 10mentioning

confidence: 97%

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Tearing up a misaligned accretion disc with a binary companion

Doğan

Nixon

King

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Accretion discs are common in binary systems, and they are often found to be misaligned with respect to the binary orbit. The gravitational torque from a companion induces nodal precession in misaligned disc orbits. We calculate whether this precession is strong enough to overcome the internal disc torques communicating angular momentum. For typical parameters precession wins: the disc breaks into distinct planes that precess effectively independently. We run hydrodynamical simulations to check these results, and confirm that disc breaking is widespread and generally enhances accretion on to the central object. This applies in many cases of astrophysical accretion, e.g. supermassive black hole binaries and X-ray binaries.

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Section: Fig 1 Shows the Simulation With An Initial Inclination Of 10mentioning

confidence: 90%

Section: Fig 1 Shows the Simulation With An Initial Inclination Of 10mentioning

confidence: 97%

Tearing up a misaligned accretion disc with a binary companion

Doğan

Nixon

King

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…In Martin et al (2014a), we found in simulations that gas capture by a binary companion appears to occur more easily if the disk is eccentric. Furthermore, substantially inclined disks can be subject to Kozai-Lidov oscillations that generate disk eccentricity (Martin et al 2014b). Consequently, the effects of disk inclination may naturally bring about additional effects due to disk eccentricity that in turn allows for greater disk extension.…”

Section: Discussionmentioning

confidence: 99%

Tidal Torques on Misaligned Disks in Binary Systems

Lubow

Martin

Nixon

2015

ApJ

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We extend previous studies of the tidal truncation of coplanar disks in binary systems to the more general case of noncoplanar disks. As in the prograde coplanar case, Lindblad resonances play a key role in tidal truncation. We analyze the tidal torque acting on a misaligned nearly circular disk in a circular orbit binary system. We concentrate on the 2:1 inner Lindblad resonance associated with the m = 2 tidal forcing (for azimuthal wavenumber m) that plays a major role in the usual coplanar case. We determine the inclination dependence of this torque, which is approximately cos 8 (i/2) for misalignment angle i. Compared to the prograde coplanar case (i = 0), this torque decreases by a factor of about 2 for i = π/6 and by a factor of about 20 for i = π/2. The Lindblad torque decreases to zero for a tilt angle of π (counter-rotation), consistent with previous investigations. The effects of higher order resonances associated with m > 2 tidal forcing may contribute somewhat, but are much more limited than in the i = 0 case. These results suggest that misaligned disks in binary systems can be significantly extended compared to their coplanar counterparts. In cases where a disk is sufficiently inclined and viscous, it can overrun all Lindblad resonances and overflow the Roche lobe of the disk central object.

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“…Recently [92] performed simulations of the KL mechanism in hydrodynamical disks around a component of a binary system, finding oscillations of the inclination angle. The persistent m = 1 structure in the disks of models NC1 can be thought of as an eccentric distribution of matter.…”

Section: G Disk Twist and Tiltmentioning

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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The Kozai-Lidov Mechanism in Hydrodynamical Disks

Cited by 157 publications

References 49 publications

Tearing up a misaligned accretion disc with a binary companion

Tearing up a misaligned accretion disc with a binary companion

Tidal Torques on Misaligned Disks in Binary Systems

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

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