<scp>Phantom</scp>: A Smoothed Particle Hydrodynamics and Magnetohydrodynamics Code for Astrophysics

Price, Daniel J.; Wurster, James; Tricco, Terrence S.; Nixon, Chris; Toupin, Stéven; Pettitt, Alex R.; Chan, Conrad; Mentiplay, Daniel; Laibe, Guillaume; Glover, Simon C. O.; Dobbs, Clare; Nealon, Rebecca; Liptai, David; Wörpel, H.; Bonnerot, Clément; Dipierro, Giovanni; Ballabio, Giulia; Ragusa, Enrico; Federrath, Christoph; Iaconi, Roberto; Reichardt, Thomas; Forgan, Duncan; Hutchison, Mark; Constantino, T.; Ayliffe, Ben; Hirsh, Kieran; Lodato, Giuseppe

doi:10.1017/pasa.2018.25

Cited by 410 publications

(359 citation statements)

References 385 publications

(1,124 reference statements)

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“…We performed 3D smoothed particle hydrodynamical (SPH) simulations using the code PHANTOM (Price et al 2018a). We explore the evolution of the gas disc, adding dust grains once the system has reached a quasi-steady state.…”

Section: Methodsmentioning

confidence: 99%

“…Given this, we scaled our code units prior to conducting the radiative transfer calculations to better match the observed cavity size in IRS 48. The code units are scaled such that the length unit was increased by 30%, and the time unit scaled by an amount to match the change in length scale, according to equation 33 in Price et al (2018a). This means that the semi-major axis of our binary companion is scaled to 13 au.…”

Section: Radiative Transfer and Synthetic Observationsmentioning

confidence: 99%

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Signatures of an eccentric disc cavity: Dust and gas in IRS 48

Calcino

Price

Pinte

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We test the hypothesis that the disc cavity in the 'transition disc' Oph IRS 48 is carved by an unseen binary companion. We use 3D dust-gas smoothed-particle hydrodynamics simulations to demonstrate that marginally coupled dust grains concentrate in the gas over-density that forms in in the cavity around a low binary mass ratio binary. This produces high contrast ratio dust asymmetries at the cavity edge similar to those observed in the disc around IRS 48 and other transition discs. This structure was previously assumed to be a vortex. However, we show that the observed velocity map of IRS 48 displays a peculiar asymmetry that is not predicted by the vortex hypothesis. We show the unusual kinematics are naturally explained by the non-Keplerian flow of gas in an eccentric circumbinary cavity. We further show that perturbations observed in the isovelocity curves of IRS 48 may be explained as the product of the dynamical interaction between the companion and the disc. The presence of a ∼0.4 M companion at a ∼10 au separation can qualitatively explain these observations. High spatial resolution line and continuum imaging should be able to confirm this hypothesis.

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Section: Methodsmentioning

confidence: 99%

Section: Radiative Transfer and Synthetic Observationsmentioning

confidence: 99%

Signatures of an eccentric disc cavity: Dust and gas in IRS 48

Calcino

Price

Pinte

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…In order to further study the behaviour of the planets embedded in the accretion disc, including the viscous evolution of the disc and higher initial inclinations, we perform Smoothed Particle Hydrodynamics (SPH) numerical simulations using the code phantom (Lodato & Price 2010;Price & Federrath 2010;Price 2012;Price et al 2017;Nixon 2012;Nixon et al 2013). Planets embedded in accretion discs around one component of a binary star system have been previously studied with phantom (e.g.…”

Section: Multi-planet Disc Hydrodynamical Simulationsmentioning

confidence: 99%

Multiplanet disc interactions in binary systems

Franchini

Martin

Lubow

2019

Monthly Notices of the Royal Astronomical Society

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We investigate the evolution of a multi-planet-disc system orbiting one component of a binary star system. The planet-disc system is initially coplanar but misaligned to the binary orbital plane. The planets are assumed to be giants that open gaps in the disc. We first study the role of the disc in shaping the mutual evolution of the two planets using a secular model for low initial tilt. In general we find that the planets and the disc do not remain coplanar, in agreement with Lubow & Martin (2016) for the single planet case. Instead, the planets and the disc undergo tilt oscillations. A high mass disc between the two planets causes the planets and the disc to nodally precess at the same average rate but they are generally misaligned. The amplitude of the tilt oscillations between the planets is larger while the disc is present. We then consider higher initial tilts using hydrodynamical simulations and explore the possibility of the formation of eccentric Kozai-Lidov (KL) planets. We find that the inner planet's orbit undergoes eccentricity growth for a large range of disc masses and initial misalignments. For a low disc mass and large initial misalignment both planets and the disc can undergo KL oscillations. Furthermore, we find that sufficiently massive discs can cause the inner planet to increase its inclination beyond 90 • and therefore to orbit the binary in a retrograde fashion. The results have important implications for the explanation of very eccentric planets and retrograde planets observed in multi-planet systems.

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“…Newer SPH flavours aim to increase the mixing of gas by altering the SPH equations (e.g. Ritchie & Thomas 2001;Read & Hayfield 2012;Hopkins 2013;Price et al 2017), and/or by adding an additional term which diffuses the entropy of particles across discontinuities (Price 2008).…”

Section: Introductionmentioning

confidence: 99%

Hydrostatic mass estimates of massive galaxy clusters: a study with varying hydrodynamics flavours and non-thermal pressure support

Pearce

Kay

Barnes

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We use a set of 45 simulated clusters with a wide mass range (8 × 10 13 < M 500 [M ] < 2×10 15 ) to investigate the effect of varying hydrodynamics flavours on cluster mass estimates. The cluster zooms were simulated using the same cosmological models as the BAHAMAS and C-EAGLE projects, leading to differences in both the hydrodynamic solvers and the subgrid physics but still producing clusters which broadly match observations. At the same mass resolution as BAHAMAS, for the most massive clusters (M 500 > 10 15 M ), we find changes in the SPH method produce the greatest differences in the final halo, while the subgrid models dominate at lower mass. By calculating the mass of all of the clusters using different permutations of the pressure, temperature and density profiles, created with either the true simulated data or mock spectroscopic data, we find that the spectroscopic temperature causes a bias in the hydrostatic mass estimates which increases with the mass of the cluster, regardless of the SPH flavour used. For the most massive clusters, the estimated mass of the cluster using spectroscopic density and temperature profiles is found to be as low as 50 per cent of the true mass compared to ∼ 90 per cent for low mass clusters. When including a correction for non-thermal pressure, the spectroscopic hydrostatic mass estimates are less biased on average and the mass dependence of the bias is reduced, although the scatter in the measurements does increase.Cluster masses can be estimated observationally using a variety of different techniques including X-ray observations, lensing and galaxy kinematics. In the first case, density and temperature profiles obtained from X-ray data are combined assuming hydrostatic equilibrium (e.g. Vikhlinin et al. 2006). However, many 1 We define M 500 as the mass of a cluster within a sphere of radius r 500 that encloses a density equal to 500 times the critical density of the Universe, ρ crit . 2 With the exception of halo 40 in this analysis which is halo 29 in the C-EAGLE sample.

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Phantom: A Smoothed Particle Hydrodynamics and Magnetohydrodynamics Code for Astrophysics

Cited by 410 publications

References 385 publications

Signatures of an eccentric disc cavity: Dust and gas in IRS 48

Signatures of an eccentric disc cavity: Dust and gas in IRS 48

Multiplanet disc interactions in binary systems

Hydrostatic mass estimates of massive galaxy clusters: a study with varying hydrodynamics flavours and non-thermal pressure support

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