Parametric instability in a free-evolving warped protoplanetary disc

Deng, Hongping; Ogilvie, Gordon I.; Mayer, Lucio

doi:10.1093/mnras/staa3504

Cited by 18 publications

(15 citation statements)

References 62 publications

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“…Several studies have argued that the most notable advantages of MFM compared to SPH or AMR methods may come in astrophysical discs, which are crucial for the physics of stellar accretion but are often marginally resolved in our simulations (meaning that more-rapid convergence at fixed resolution is especially valuable). For example, (1) MFM accurately conserves angular momentum and prevents both unphysical disc 'spreading' and/or clumping/fragmentation via artificial viscous instabilities in SPH or catastrophic angular momentum loss from spurious coordinatealignment torques which are inescapable in AMR (Hopkins 2015;Few et al 2016;Zhu & Li 2016;Lupi et al 2017;Panuelos et al 2020;Deng, Ogilvie & Mayer 2021). ( 2) Few et al (2016) found MFM more rapidly converges to correct linear growth rates for spiral arms and other disc instabilities, compared to AMR or SPH, while Deng et al (2021) found a similar result for physical parametric instabilities of warped discs.…”

Section: Existing Testsmentioning

confidence: 93%

“…For example, (1) MFM accurately conserves angular momentum and prevents both unphysical disc 'spreading' and/or clumping/fragmentation via artificial viscous instabilities in SPH or catastrophic angular momentum loss from spurious coordinatealignment torques which are inescapable in AMR (Hopkins 2015;Few et al 2016;Zhu & Li 2016;Lupi et al 2017;Panuelos et al 2020;Deng, Ogilvie & Mayer 2021). ( 2) Few et al (2016) found MFM more rapidly converges to correct linear growth rates for spiral arms and other disc instabilities, compared to AMR or SPH, while Deng et al (2021) found a similar result for physical parametric instabilities of warped discs. (3) Deng, Mayer & Meru (2017) showed MFM was the only method surveyed which exhibited convergence to exact solutions for gravitoturbulent fragmentation in cooling discs.…”

Section: Existing Testsmentioning

confidence: 99%

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STARFORGE: Towards a comprehensive numerical model of star cluster formation and feedback

Grudić

Guszejnov

Hopkins

et al. 2021

Monthly Notices of the Royal Astronomical Society

115

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We present STARFORGE (STAR FORmation in Gaseous Environments): a new numerical framework for 3D radiation MHD simulations of star formation that simultaneously follow the formation, accretion, evolution, and dynamics of individual stars in massive giant molecular clouds (GMCs) while accounting for stellar feedback, including jets, radiative heating and momentum, stellar winds, and supernovae. We use the GIZMO code with the MFM mesh-free Lagrangian MHD method, augmented with new algorithms for gravity, timestepping, sink particle formation and accretion, stellar dynamics, and feedback coupling. We survey a wide range of numerical parameters/prescriptions for sink formation and accretion and find very small variations in star formation history and the IMF (except for intentionally-unphysical variations). Modules for mass-injecting feedback (winds, SNe, and jets) inject new gas elements on-the-fly, eliminating the lack of resolution in diffuse feedback cavities otherwise inherent in Lagrangian methods. The treatment of radiation uses GIZMO’s radiative transfer solver to track 5 frequency bands (IR, optical, NUV, FUV, ionizing), coupling direct stellar emission and dust emission with gas heating and radiation pressure terms. We demonstrate accurate solutions for SNe, winds, and radiation in problems with known similarity solutions, and show that our jet module is robust to resolution and numerical details, and agrees well with previous AMR simulations. STARFORGE can scale up to massive (>105M⊙) GMCs on current supercomputers while predicting the stellar (≳ 0.1M⊙) range of the IMF, permitting simulations of both high- and low-mass cluster formation in a wide range of conditions.

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Section: Existing Testsmentioning

confidence: 93%

Section: Existing Testsmentioning

confidence: 99%

STARFORGE: Towards a comprehensive numerical model of star cluster formation and feedback

Grudić

Guszejnov

Hopkins

et al. 2021

Monthly Notices of the Royal Astronomical Society

115

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show abstract

“…Indeed, a variety of other effects might modify our solution families, including the parametric instability proposed by Gammie et al (2000). This has been shown to be active in global disc simulations by Deng et al (2021) and may present an enhanced turbulent viscosity affecting the evolution of our periodic modes. In the future, we propose setting up numerical simulations which target the internal flow structure of warped discs and test how robust they are in the presence of more general physics.…”

Section: Discussionmentioning

confidence: 92%

Non-linear resonant torus oscillations as a model of Keplerian disc warp dynamics

Fairbairn

Ogilvie

2021

Monthly Notices of the Royal Astronomical Society

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Observations of distorted discs have highlighted the ubiquity of warps in a variety of astrophysical contexts. This has been complemented by theoretical efforts to understand the dynamics of warp evolution. Despite significant efforts to understand the dynamics of warped discs, previous work fails to address arguably the most prevalent regime – nonlinear warps in Keplerian discs for which there is a resonance between the orbital, epicyclic and vertical oscillation frequencies. In this work, we implement a novel nonlinear ring model, developed recently by Fairbairn and Ogilvie, as a framework for understanding such resonant warp dynamics. Here we uncover two distinct nonlinear regimes as the warp amplitude is increased. Initially we find a smooth modulation theory which describes warp evolution in terms of the averaged Lagrangian of the oscillatory vertical motions of the disc. This hints towards the possibility of connecting previous warp theory under a generalised secular framework. Upon the warp amplitude exceeding a critical value, which scales as the square root of the aspect-ratio of our ring, the disc enters into a bouncing regime with extreme vertical compressions twice per orbit. We develop an impulsive theory which predicts special retrograde and prograde precessing warped solutions, which are identified numerically using our full equation set. Such solutions emphasise the essential activation of nonlinear vertical oscillations within the disc and may have important implications for energy and warp dissipation. Future work should search for this behaviour in detailed numerical studies of the internal flow structure of warped discs.

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“…This increase in resolution leads to a corresponding drop in the viscosity arising from numerical viscosity. We 5 One possibility to significantly increase the local resolution without significantly increasing the computational cost is to perform local ("shearing box") simulations and these have been employed to explore detailed internal dynamics in warped disc (see, for example, Ogilvie & Latter 2013b; Deng et al 2021), but such simulations cannot be directly applied to determine the global behaviour of the disc with regards to disc breaking or radial tilt oscillations. 6 It is worth remarking that found, contrary to the prediction of a local stability analysis (Dogan et al 2018), that the growth rates of the instability in unstable disc regions were relatively insensitive to the level of the viscosity.…”

Section: Results Presented Herementioning

confidence: 99%

“…Gammie et al 2000) which have been followed up with targetted numerical simulations (e.g. Paardekooper & Ogilvie 2019;Deng et al 2021).…”

Section: Introductionmentioning

confidence: 99%

On the dynamics of low-viscosity warped discs around black holes

Drewes,

Nixon

2021

Preprint

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Accretion discs around black holes can become warped by Lense-Thirring precession if the disc is tilted with respect to the black hole spin vector. When the disc viscosity is sufficiently large that warp propagation is diffusive, the inner disc can align with the black hole spin. However, if the viscosity is small, such that the warp propagates as a wave, then steady-state solutions to the linearised fluid equations exhibit an oscillatory radial profile of the disc tilt angle close to the black hole. Here we show, for the first time, that these solutions are in good agreement with three-dimensional hydrodynamical simulations, in which the viscosity is isotropic and measured to be small compared to the disc angular semi-thickness, and in the case that the disc tilt-and thus the warp amplitude-remains small. We show using both the linearised fluid equations and hydrodynamical simulations that the inner disc tilt can be more than several times larger than the original disc tilt, and we provide physical reasoning for this effect. We explore the transition in disc behaviour as the misalignment angle is increased, finding increased dissipation associated with regions of strong warping. For large enough misalignments the disc becomes unstable to disc tearing and breaks into discrete planes. For the simulations we present here, we show that the total (physical and numerical) viscosity at the time the disc breaks is small enough that the disc tearing occurs in the wave-like regime, substantiating that disc tearing is possible in this region of parameter space. Our simulations demonstrate that high spatial resolution, and thus low numerical viscosity, is required to accurately model the warp dynamics in this regime. Finally, we discuss the observational implications of our results.

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Parametric instability in a free-evolving warped protoplanetary disc

Cited by 18 publications

References 62 publications

STARFORGE: Towards a comprehensive numerical model of star cluster formation and feedback

STARFORGE: Towards a comprehensive numerical model of star cluster formation and feedback

Non-linear resonant torus oscillations as a model of Keplerian disc warp dynamics

On the dynamics of low-viscosity warped discs around black holes

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