Accretional evolution of a planetesimal swarm: 1. A new simulation

Spaute, D.; Weidenschilling, S. J.; Davis, Donald R.; Marzari, F.

doi:10.1016/0019-1035(91)90041-q

Cited by 81 publications

(104 citation statements)

References 20 publications

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“…where β = 1 for a pure two body interaction and β ≈ 2.7 accounts for anisotropic effects introduced by orbital dynamics (Greenzweig & Lissauer 1990;Spaute et al 1991;Wetherill & Stewart 1993). Putting these results together and ignoring order unity coefficients gives the dispersion-dominated growth timescale m l /ṁ l as…”

Section: Gravitationally Focused Collisionsmentioning

confidence: 99%

“…Several hybrid codes combine aspects of both approaches (Spaute et al 1991;Weidenschilling et al 1997;Bromley & Kenyon 2006;Charnoz & Morbidelli 2007;Raymond et al 2011). To follow the evolution of the gaseous disk together with the solids, Bromley & Kenyon (2011) solve the radial diffusion equation for the gaseous disk (eq.…”

Section: Numerical Simulations Of Low Mass Planet Formationmentioning

confidence: 99%

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From Disks to Planets

Youdin

Kenyon

2013

Planets, Stars and Stellar Systems

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This pedagogical chapter covers the theory of planet formation, with an emphasis on the physical processes relevant to current research. After summarizing empirical constraints from astronomical and geophysical data, we describe the structure and evolution of protoplanetary disks. We consider the growth of planetesimals and of larger solid protoplanets, followed by the accretion of planetary atmospheres, including the core accretion instability. We also examine the possibility that gas disks fragment directly into giant planets and/or brown dwarfs. We defer a detailed description of planet migration and dynamical evolution to other work, such as the complementary chapter in this series by Morbidelli (available at arXiv:1106.4114).Comment: 50 pages text plus 11 figures and table of symbols. To be published in "Planets, Stars and Stellar Systems", P. Kalas and L. French (eds.). Comments and suggestions for future revisions welcom

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Section: Gravitationally Focused Collisionsmentioning

confidence: 99%

Section: Numerical Simulations Of Low Mass Planet Formationmentioning

confidence: 99%

From Disks to Planets

Youdin

Kenyon

2013

Planets, Stars and Stellar Systems

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“…This is a distinct feature of our approach: usually, coordinates and velocities in a corotating "box" are used instead (e.g. Greenberg et al 1978;Spaute et al 1991;Weidenschilling et al 1997). To accommodate systems where large eccentricites and/or inclination cause large radial and/or vertical excursions of particles, standard codes employ multiannulus schemes, whereas our approach treats such cases in a straightforward way.…”

Section: Kinetic Theory In Orbital Elementsmentioning

confidence: 99%

Dust distributions in debris disks: effects of gravity, radiation pressure and collisions

Krivov¹,

Löhne²,

Sremčević

2006

A&A

182

308

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We model a typical debris disk, treated as an idealized ensemble of dust particles, exposed to stellar gravity and direct radiation pressure and experiencing fragmenting collisions. Applying the kinetic method of statistical physics, written in orbital elements, we calculate size and spatial distibutions expected in a steady-state disk, investigate timescales needed to reach the steady state, and calculate mass loss rates. Particular numerical examples are given for the debris disk around Vega. The disk should comprise a population of larger grains in bound orbits and a population of smaller particles in hyperbolic orbits. The cross section area is dominated by the smallest grains that still can stay in bound orbits, for Vega about 10 µm in radius. The size distribution is wavy, implying secondary peaks in the size distribution at larger sizes. The radial profile of the pole-on surface density or the optical depth in the steady-state disk has a power-law index between about −1 and −2. It cannot be much steeper even if dust production is confined to a narrow planetesimal belt, because collisional grinding produces smaller and smaller grains, and radiation pressure pumps up their orbital eccentricities and spreads them outward, which flattens the radial profile. The timescales to reach a steady state depend on grain sizes and distance from the star. For Vega, they are about 1 Myr for grains up to some hundred µm at 100 AU. The total mass of the Vega disk needed to produce the observed amount of micron and submillimeter-sized dust does not exceed several earth masses for an upper size limit of parent bodies of about 1 km. The collisional depletion of the disk occurs on Gyr timescales.

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“…There have been a couple of attempts at constructing an end-to-end simulation of planet formation that started with a population of small planetesimals and built a complete planetary system (Spaute et al 1991;Weidenschilling et al 1997; Kenyon & Bromley 2006;Bromley & Kenyon 2011, for example). These have employed codes that graft an N-body algorithm onto Eulerian statistical code.…”

Section: Introductionmentioning

confidence: 99%

A Lagrangian Integrator for Planetary Accretion and Dynamics (Lipad)

Levison

Duncan

Thommes

2012

The Astronomical Journal

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We present the first particle-based Lagrangian code that can follow the collisional/accretional/dynamical evolution of a large number of kilometer-sized planetesimals through the entire growth process of becoming planets. We refer to it as the Lagrangian Integrator for Planetary Accretion and Dynamics or LIPAD. LIPAD is built on top of SyMBA, which is a symplectic N-body integrator. In order to handle the very large number of planetesimals required by planet formation simulations, we introduce the concept of a tracer particle. Each tracer is intended to represent a large number of disk particles on roughly the same orbit and size as one another and is characterized by three numbers: the physical radius, the bulk density, and the total mass of the disk particles represented by the tracer. We developed statistical algorithms that follow the velocity and size evolution of the tracers due to close gravitational encounters and physical collisions with one another. The tracers mainly dynamically interact with the larger objects (planetary embryos) in the normal N-body way. LIPAD's greatest strength is that it can accurately model the wholesale redistribution of planetesimals due to gravitational interaction with the embryos, which has recently been shown to significantly affect the growth rate of planetary embryos. We verify the code via a comprehensive set of tests that compare our results with those of Eulerian and/or direct N-body codes.

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Accretional evolution of a planetesimal swarm: 1. A new simulation

Cited by 81 publications

References 20 publications

From Disks to Planets

From Disks to Planets

Dust distributions in debris disks: effects of gravity, radiation pressure and collisions

A Lagrangian Integrator for Planetary Accretion and Dynamics (Lipad)

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