Smoothed particle hydrodynamics simulations of gas and dust mixtures

Booth, Richard A; Sijacki, Debora; Clarke, C. J.

doi:10.1093/mnras/stv1486

Cited by 47 publications

(58 citation statements)

References 55 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…giving the same solution as Equation 6. This regime corresponds to the short friction time approximation used to estimate the terminal velocity of the dust in many studies (Johansen & Klahr 2005;Booth et al 2015;Lin & Youdin 2017). To conclude, the drag force source term in the equations of conservation of movement can be expressed as…”

Section: Equations Of Coupled Fluidsmentioning

confidence: 99%

Dust-vortex Instability in the Regime of Well-coupled Grains

Surville

Mayer

2019

ApJ

View full text Add to dashboard Cite

We present a novel study of dust-vortex evolution in global two-fluid disk simulations to find out if evolution toward high dust-to-gas ratios can occur in a regime of well-coupled grains with low Stokes numbers (St = 10 −3 − 4 × 10 −2 ). We design a new implicit scheme in the code RoSSBi, to overcome the short timesteps occurring for small grain sizes. We discover that the linear capture phase occurs self-similarly for all grain sizes, with an intrinsic timescale (characterizing the vortex lifetime) scaling as 1/St. After vortex dissipation, the formation of a global active dust ring is a generic outcome confirming our previous results obtained for larger grains. We propose a scenario in which, irrespective of grain size, multiple pathways can lead to local dust-to-gas ratios of order unity and above on relatively short timescales, < 10 5 yr, in the presence of a vortex, even with St = 10 −3 . When St > 10 −2 , the vortex is quickly dissipated by two-fluid instabilities, and large dust density enhancements form in the global dust ring. When St < 10 −2 , the vortex is resistant to destabilization. As a result, dust concentrations occur locally due to turbulence developing inside the vortex. Whatever the Stokes number, dust-to-gas ratios in the range 1 − 10, a necessary condition to trigger a subsequent streaming instability, or even a direct gravitational instability of the dust clumps, appears to be an inevitable outcome. Although quantitative connections with other instabilities still need to be made, we argue that our results support a new scenario of vortex-driven planetesimal formation.

show abstract

Section: Equations Of Coupled Fluidsmentioning

confidence: 99%

Dust-vortex Instability in the Regime of Well-coupled Grains

Surville

Mayer

2019

ApJ

View full text Add to dashboard Cite

show abstract

“…We emphasize that it is important to adopt a scheme that can correctly follow the supersonic drag force. For example, semi-analytic methods such as those proposed by Booth, Sijacki & Clarke (2015) and Lorén-Aguilar & Bate (2015), which only apply for the subsonic cases, will predict solutions that significantly underestimate the drag force, as shown in Fig. 2.…”

Section: Validationmentioning

confidence: 99%

Thermal and non-thermal dust sputtering in hydrodynamical simulations of the multiphase interstellar medium

Zhukovska

Somerville

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We study the destruction of interstellar dust via sputtering in supernova (SN) shocks using three-dimensional hydrodynamical simulations. With a novel numerical framework, we follow both sputtering and dust dynamics governed by direct collisions, plasma drag and betatron acceleration. Grain-grain collisions are not included and the grain-size distribution is assumed to be fixed. The amount of dust destroyed per SN is quantified for a broad range of ambient densities and fitting formulae are provided. Integrated over the grain-size distribution, nonthermal (inertial) sputtering dominates over thermal sputtering for typical ambient densities. We present the first simulations that explicitly follow dust sputtering within a turbulent multiphase interstellar medium. We find that the dust destruction timescales τ are 0.35 Gyr for silicate dust and 0.44 Gyr for carbon dust in solar neighborhood conditions. The SN environment has an important impact on τ . SNe that occur in preexisting bubbles destroy less dust as the destruction is limited by the amount of dust in the shocked gas. This makes τ about 2.5 times longer than the estimate based on results from a single SN explosion. We investigate the evolution of the dust-to-gas mass ratio (DGR), and find that a spatial inhomogeneity of ∼ 14% develops for scales below 10 pc. It locally correlates positively with gas density but negatively with gas temperature even in the exterior of the bubbles due to incomplete gas mixing. This leads to a ∼ 30% lower DGR in the volume filling warm gas compared to that in the dense clouds.

show abstract

“…An improved approach would be to model the dust as a separate fluid (e.g. Bekki 2015;Booth et al 2015;McKinnon et al 2018) and then assess how coupled the dust grains and gas remain in the presence of the strong shocks driven by radiative AGN feedback.…”

Section: Dust Physicsmentioning

confidence: 99%

Radiative AGN feedback on a moving mesh: the impact of the galactic disc and dust physics on outflow properties

Barnes

Kannan

Vogelsberger

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Feedback from accreting supermassive black holes, active galactic nuclei (AGN), is now a cornerstone of galaxy formation models. In this work, we present radiation-hydrodynamic simulations of radiative AGN feedback using the novel AREPO-RT code. A central black hole emits radiation at a constant luminosity and drives an outflow via radiation pressure on dust grains. Utilising an isolated NFW halo we validate our setup in the single and multi-scattering regimes, with the simulated shock front propagation in excellent agreement with the expected analytic result. For a spherically symmetric NFW halo, an examination of the simulated outflow properties generated by radiative feedback demonstrates that they are lower than typically observed at a fixed AGN luminosity, regardless of the collimation of the radiation. We then explore the impact of a central disc galaxy and the assumed dust model on the outflow properties. The contraction of the halo during the galaxy's formation and modelling the production of dust grains results in a factor 100 increase in the halo's optical depth. Radiation is then able to couple momentum more efficiently to the gas, driving a stronger shock and producing a mass-loaded ∼ 10 3 M yr −1 outflow with a velocity of ∼ 2000 km s −1 , in agreement with observations. However, the inclusion of dust destruction mechanisms, like thermal sputtering, leads to the rapid destruction of dust grains within the outflow, reducing its properties below typically observed values. We conclude that radiative AGN feedback can drive outflows, but a thorough numerical and physical treatment is required to assess its true impact.

show abstract

Smoothed particle hydrodynamics simulations of gas and dust mixtures

Cited by 47 publications

References 55 publications

Dust-vortex Instability in the Regime of Well-coupled Grains

Dust-vortex Instability in the Regime of Well-coupled Grains

Thermal and non-thermal dust sputtering in hydrodynamical simulations of the multiphase interstellar medium

Radiative AGN feedback on a moving mesh: the impact of the galactic disc and dust physics on outflow properties

Contact Info

Product

Resources

About