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

@article{Krivov2006DustDI,
  title={Dust distributions in debris disks: effects of gravity, radiation pressure and collisions},
  author={Alexander V. Krivov and Torsten L{\"o}hne and Miodrag Sremčević},
  journal={Astronomy and Astrophysics},
  year={2006},
  volume={455},
  pages={509-519}
}
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… 

Long-Term Collisional Evolution of Debris Disks

IR surveys indicate that the dust content in debris disks gradually declines with stellar age. We simulated the long-term collisional depletion of debris disks around solar-type (G2 V) stars with our

DIAGNOSING CIRCUMSTELLAR DEBRIS DISKS

A numerical model of a circumstellar debris disk is developed and applied to observations of the circumstellar dust orbiting β Pictoris. The model accounts for the rates at which dust is produced by

WILL NEW HORIZONS SEE DUST CLUMPS IN THE EDGEWORTH–KUIPER BELT?

Debris disks are thought to be sculptured by neighboring planets. The same is true for the Edgeworth–Kuiper debris disk, yet no direct observational evidence for signatures of giant planets in the

DEBRIS DISK SIZE DISTRIBUTIONS : STEADY STATE COLLISIONAL EVOLUTION WITH PR 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

Solution to the debris disc mass problem: planetesimals are born small?

Debris belts on the periphery of planetary systems, encompassing the region occupied by planetary orbits, are massive analogues of the Solar system's Kuiper belt. They are detected by thermal

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

The Effect of Dust Composition and Shape on Radiation-pressure Forces and Blowout Sizes of Particles in Debris Disks

The light scattered from dust grains in debris disks is typically modeled as compact spheres using the Lorenz–Mie theory or as porous spheres by incorporating an effective medium theory. In this work

Grain size segregation in debris discs

In most debris discs, dust grain dynamics is strongly affected by stellar radiation pressure. As this mechanism is size-dependent, we expect dust grains to be spatially segregated according to their

Collisional processes and size distribution in spatially extended debris discs

Context. New generations of instruments provide, or are about to provide, pan-chromatic images of debris discs and photometric measurements, that require new generations of models, in particular to

CONSTRAINTS ON PLANETESIMAL COLLISION MODELS IN DEBRIS DISKS

Observations of debris disks offer a window into the physical and dynamical properties of planetesimals in extrasolar systems through the size distribution of dust grains. In particular, the
...

References

SHOWING 1-10 OF 46 REFERENCES

Dust Migration and Morphology in Optically Thin Circumstellar Gas Disks

We analyze the dynamics of gas-dust coupling in the presence of stellar radiation pressure in circumstellar disks, which are in a transitional stage between the gas-dominated, optically thick,

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

Prospects for Detection of Catastrophic Collisions in Debris Disks

We investigate the prospects for detecting dust from two-body collisions during the late stages of planet formation at 1–150 AU. We develop an analytic model to describe the formation of a dusty

Signatures of Exosolar Planets in Dust Debris Disks

We apply our recently elaborated, powerful numerical approach to the high-resolution modeling of the structure and emission of circumstellar dust disks, incorporating all relevant physical processes.

A Study of the Dynamics of Dust from the Kuiper Belt: Spatial Distribution and Spectral Energy Distribution

The dust produced in the Kuiper belt (KB) spreads throughout the solar system, forming a dust disk. We numerically model the orbital evolution of KB dust and estimate its equilibrium spatial

Collisional processes in extrasolar planetesimal discs – dust clumps in Fomalhaut's debris disc

This paper presents a model for the outcome of collisions between planetesimals in a debris disc, and assesses the impact of collisional processes on the structure and size distribution of the disc.

Upper limit on the gas density in the β Pictoris system

We investigate the effect of gas drag on the dynamics of the dust particles in the edge-on β Pictoris disc to derive an upper limit on the mass of gas in this system. Our study is motivated by the

Quasi-Stationary States of Dust Flows under Poynting-Robertson Drag: New Analytical and Numerical Solutions

The effect of solar or stellar radiation on dust particles' trajectories (the Poynting-Robertson drag) has been studied by a number of authors and applied to interplanetary dust dynamics in numerical

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