Dusty hypersonic flows

We present Phantom, a fast, parallel, modular and low-memory smoothed particle hydrodynamics and magnetohydrodynamics code developed over the last decade for astrophysical applications in three dimensions. The code has been developed with a focus on stellar, galactic, planetary and high energy astrophysics and has already been used widely for studies of accretion discs and turbulence, from the birth of planets to how black holes accrete. Here we describe and test the core algorithms as well as modules for magnetohydrodynamics, self-gravity, sink particles, dust-gas mixtures, H2 chemistry, physical viscosity, external forces including numerous galactic potentials, Lense-Thirring precession, Poynting-Robertson drag and stochastic turbulent driving. Phantom is hereby made publicly available.

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“…where the coefficient C D is given by (Fassio & Probstein, 1970) (see Whipple 1972;Weidenschilling 1977)…”

Section: Epstein Dragmentioning

confidence: 99%

Phantom: A Smoothed Particle Hydrodynamics and Magnetohydrodynamics Code for Astrophysics

Price

Wurster

Tricco

et al. 2018

Publ. Astron. Soc. Aust.

398

343

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“…The stopping time depends on the radius of the aggregates a and the particle Reynolds number Re p = 2av/ν m . The stopping time t s is given by Probstein & Fassio (1970) and Weidenschilling (1977) as follows. If the radius of an aggregate a is smaller than (9/4)λ m , then the stopping time of the dust aggregates is determined by Epstein's law, t Ep s = 3m/(4πρ g v th a 2 ).…”

Section: Turbulent Motionsmentioning

confidence: 99%

Ejection of Chondrules from Fluffy Matrices

Arakawa

2017

ApJ

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Chondritic meteorites primarily contain millimeter-sized spherical objects, the so-called chondrules; however, the co-accretion process of chondrules and matrix grains is not yet understood. In this study, we investigate the ejection process of chondrules via collisions of fluffy aggregates composed of chondrules and matrices. We reveal that fluffy aggregates cannot grow into planetesimals without losing chondrules if we assume that the chondrite parent bodies are formed via direct aggregation of similar-sized aggregates. Therefore, an examination of other growth pathways is necessary to explain the formation of rocky planetesimals in our solar system.

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“…The Stokes approximation begins to fail significantly for R e > 10, but the drag force is overestimated only by about a factor of 3 at R e = 10 2 . (See Probstein and Fassio, 1969. ) An inertia parameter \p is defined as…”

Section: Impact Of Small Particles On a Sphere Moving Through A Gasmentioning

confidence: 99%

“…Fuchs (1964) and Soo (1967) summarized the subject for subsonic flow and included both theoretical and experimental results by various investigators. Probstein and Fassio (1969) investigated "dusty hypersonic flows." The transonic case has apparently not been attacked seriously.…”

mentioning

confidence: 99%

Accumulation of Chondrules on Asteroids

Whipple

1971

International Astronomical Union Colloquium

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It is suggested that aerodynamic forces played a significant role in the selective accumulation of chondrules on asteroids moving with respect to the gas in a primeval solar nebula. Particles smaller than millimeter chondrules would sweep by an asteroid moving in a critical velocity range, whereas larger particles could be accumulated by impact. Theory and calculation cover the case of subsonic velocity and asteroidal diameter up to 50 km for a nebula density up to 10-6 g/cm3, or higher for smaller asteroids.

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Dusty hypersonic flows

Cited by 53 publications

References 2 publications

Phantom: A Smoothed Particle Hydrodynamics and Magnetohydrodynamics Code for Astrophysics

Phantom: A Smoothed Particle Hydrodynamics and Magnetohydrodynamics Code for Astrophysics

Ejection of Chondrules from Fluffy Matrices

Accumulation of Chondrules on Asteroids

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