A NEW ALGORITHM FOR SELF-CONSISTENT THREE-DIMENSIONAL MODELING OF COLLISIONS IN DUSTY DEBRIS DISKS

@article{Stark2009ANA,
  title={A NEW ALGORITHM FOR SELF-CONSISTENT THREE-DIMENSIONAL MODELING OF COLLISIONS IN DUSTY DEBRIS DISKS},
  author={Christopher C. Stark and Marc J. Kuchner},
  journal={The Astrophysical Journal},
  year={2009},
  volume={707},
  pages={543 - 553}
}
We present a new “collisional grooming” algorithm that enables us to model images of debris disks where the collision time is less than the Poynting–Robertson (PR) time for the dominant grain size. Our algorithm uses the output of a collisionless disk simulation to iteratively solve the mass flux equation for the density distribution of a collisional disk containing planets in three dimensions. The algorithm can be run on a single processor in ∼1 hr. Our preliminary models of disks with… 

SMACK: A NEW ALGORITHM FOR MODELING COLLISIONS AND DYNAMICS OF PLANETESIMALS IN DEBRIS DISKS

We present the Superparticle-Method/Algorithm for Collisions in Kuiper belts and debris disks (SMACK), a new method for simultaneously modeling, in three dimensions, the collisional and dynamical

A new code to study structures in collisionally active, perturbed debris discs: application to binaries

Debris discs are traditionally studied using two distinct types of numerical models: statistical particle-in-a-box codes to study their collisional and size distribution evolution, and dynamical

GAP CLEARING BY PLANETS IN A COLLISIONAL DEBRIS DISK

We apply our 3D debris disk model, SMACK, to simulate a planet on a circular orbit near a ring of planetesimals that are experiencing destructive collisions. Previous simulations of a planet opening

COLLISIONAL GROOMING MODELS OF THE KUIPER BELT DUST CLOUD

We modeled the three-dimensional structure of the Kuiper Belt (KB) dust cloud at four different dust production rates, incorporating both planet–dust interactions and grain–grain collisions using the

A SMACK MODEL OF COLLIDING PLANETESIMALS IN THE β PICTORIS DEBRIS DISK

We present a new model of the β Pictoris disk-and-planet system that simulates both the planetesimal collisions and the dynamics of the resulting dust grains, allowing us to model features and

Debris disk size distributions: steady state collisional evolution with Poynting-Robertson drag and other loss processes

We present a new scheme for determining the shape of the size distribution, and its evolution, for collisional cascades of planetesimals undergoing destructive collisions and loss processes like

Signatures of massive collisions in debris discs A self-consistent numerical model

Context. Violent stochastic collisional events have been invoked as a possible explanation for some debris discs displaying pronounced azimuthal asymmetries or having a luminosity excess exceeding

LIDT-DD: A new self-consistent debris disc model that includes radiation pressure and couples dynamical and collisional evolution

Context. In most current debris disc models, the dynamical and the collisional evolutions are studied separately with N-body and statistical codes, respectively, because of stringent computational

Planet signatures and Size Segregation in Debris Discs

  • P. Thebault
  • Physics, Geology
    Proceedings of the International Astronomical Union
  • 2013
The response of a debris disc to a planetary perturber is the result of the complex interplay between gravitational effects, grain collisions and stellar radiation pressure (Stark & Kuchner (2009).

On the cavity of a debris disc carved by a giant planet

One possible explanation of the cavity in debris discs is the gravitational perturbation of an embedded giant planet. Planetesimals passing close to a massive body are dynamically stirred resulting
...

References

SHOWING 1-10 OF 34 REFERENCES

Steady State Evolution of Debris Disks around A Stars

This paper confronts a simple analytical model for the steady state evolution of debris disks due to collisions with Spitzer observations of dust around main-sequence A stars. It is assumed that

Dust production from collisions in extrasolar planetary systems. The inner beta Pictoris disc

Dust particles observed in extrasolar planetary discs originate from undetectable km-sized bodies but this valuable information remains uninteresting if the theoretical link between grains and

Collisional dust avalanches in debris discs

We quantitatively investigate how collisional avalanches may develop in debris discs as the result of the initial breakup of a planetesimal or comet-like object, triggering a collisional chain

Collisional model of asteroids and their debris

A model for colliding objects in the asteroidal belt is formulated. An integro-differential equation describing the evolution of a system of particles undergoing inelastic collisions and

A planetary system as the origin of structure in Fomalhaut's dust belt

The sharp inner edge and offset demonstrate the presence of planetary-mass objects orbiting Fomalhaut, demonstrating the structure of a dusty disk modified by the gravitational influence of planets.

Predictions for a planet just inside Fomalhaut's eccentric ring

We propose that the eccentricity and sharpness of the edge of Fomalhaut’s disk are due to a planet just interior to the ring edge. The collision timescale consistent with the disk opacity is long

Planetesimals to protoplanets – II. Effect of debris on terrestrial planet formation

In this paper, we extend our numerical method for simulating terrestrial planet formation to include dynamical friction from the unresolved debris component. In the previous work, we implemented a

The Dynamical Influence of a Planet at Semimajor Axis 3.4 AU on the Dust around ϵ Eridani

Precise Doppler experiments suggest that a massive (m sin i = 0.86MJ) planet orbits at semimajor axis a = 3.4 AU around ϵ Eri, a nearby star with a massive debris disk. The dynamical perturbations