# Gap Clearing by Planets in a Collisional Debris Disk

@article{Nesvold2014GapCB,
title={Gap Clearing by Planets in a Collisional Debris Disk},
author={Erik Nesvold and Marc J. Kuchner},
journal={The Astrophysical Journal},
year={2014},
volume={798},
pages={83}
}
• Published 28 October 2014
• Physics, Geology
• The Astrophysical Journal
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 a gap in a collisionless debris disk have found that the width of the gap scales as the planet mass to the 2/7th power (α = 2/7). We find that gap sizes in a collisional disk still obey a power law scaling with planet mass, but that the index α of the power law depends on the age of the system t…
41 Citations

## Figures and Tables from this paper

On the cavity of a debris disc carved by a giant planet
• Physics, Geology
• 2018
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
Detection and Characterization of Extrasolar Planets through Mean-Motion Resonances: Simulations of Hypothetical Debris Disks
• Physics, Geology
• 2015
The gravitational influence of a planet on a nearby disk provides a powerful tool for detecting and studying extrasolar planetary systems. Here we demonstrate that gaps can be opened in dynamically
Impact of planetesimal eccentricities and material strength on the appearance of eccentric debris disks
• Physics, Geology
Astronomy & Astrophysics
• 2018
Context. Since circumstellar dust in debris disks is short-lived, dust-replenishing requires the presence of a reservoir of planetesimals. These planetesimals in the parent belt of debris disks orbit
Giant Planets Can Act As Stabilizing Agents on Debris Disks
• Physics, Geology
• 2017
We have explored the evolution of a cold debris disk under the gravitational influence of dwarf planet sized objects (DPs), both in the presence and absence of an interior giant planet. Through
Formation of Gaps in Self-gravitating Debris Disks by Secular Resonance in a Single-planet System. I. A Simplified Model
• Physics, Geology
• 2020
Spatially resolved images of debris disks frequently reveal complex morphologies such as gaps, spirals, and warps. Most existing models for explaining such morphologies focus on the role of massive
A SMACK MODEL OF COLLIDING PLANETESIMALS IN THE β PICTORIS DEBRIS DISK
• Physics, Geology
• 2015
We present a new model of the $\beta$ 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
Collision rates of planetesimals near mean-motion resonances
• Physics, Geology
• 2021
In circumstellar discs, collisional grinding of planetesimals produces second-generation dust. While it remains unclear whether this ever becomes a major component of the total dust content, the
The unseen planets of double belt debris disc systems
• Physics, Geology
• 2016
The gap between two component debris disks is often taken to be carved by intervening planets scattering away the remnant planetesimals. We employ N-body simulations to determine how the time needed
Numerical predictions for planets in the debris discs of HD 202628 and HD 207129
• Geology, Physics
• 2016
Resolved debris disc images can exhibit a range of radial and azimuthal structures, including gaps and rings, which can result from planetary companions shaping the disc by their gravitational
Circumstellar Debris Disks: Diagnosing the Unseen Perturber
• Physics, Geology
• 2016
The first indication of the presence of a circumstellar debris disk is usually the detection of excess infrared emission from the population of small dust grains orbiting the star. This dust is

## References

SHOWING 1-10 OF 73 REFERENCES
Resonant Structures in Planetesimal Disks due to Planetary Migration
• Physics, Geology
• 2007
Context. The observed clumpy structures in debris disks are commonly interpreted as particles trapped in mean-motion resonances with an unseen exo-planet. Populating the resonances requires a
PREDICTIONS FOR SHEPHERDING PLANETS IN SCATTERED LIGHT IMAGES OF DEBRIS DISKS
• Geology, Physics
• 2013
Planets can affect debris disk structure by creating gaps, sharp edges, warps, and other potentially observable signatures. However, there is currently no simple way for observers to deduce a
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
COLLISIONAL CASCADES IN PLANETESIMAL DISKS. II. EMBEDDED PLANETS
• Physics, Geology
• 2004
We use a multiannulus planetesimal accretion code to investigate the growth of icy planets in the outer regions of a planetesimal disk. In a quiescent minimum-mass solar nebula, icy planets grow to
SMACK: A NEW ALGORITHM FOR MODELING COLLISIONS AND DYNAMICS OF PLANETESIMALS IN DEBRIS DISKS
• Physics, Geology
• 2013
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
RESONANT TRAPPING OF PLANETESIMALS BY PLANET MIGRATION: DEBRIS DISK CLUMPS AND VEGA'S SIMILARITY TO THE SOLAR SYSTEM
This paper describes a model that can explain the observed clumpy structures of debris disks. Clumps arise because after a planetary system forms, its planets migrate because of angular momentum
A New Algorithm for Self-consistent Three-dimensional Modeling of Collisions in Dusty Debris Disks
• Physics, Geology
• 2009
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.
Chaotic zone boundary for low free eccentricity particles near an eccentric planet
We consider particles with low free or proper eccentricity that are orbiting near planets on eccentric orbits. Through collisionless particle integration, we numerically find the location of the
Perturbations of a Planet on the β Pictoris Circumstellar Dust Disk: 3. Time Scale of Collisional Destruction versus Resonance Time Scale
• Physics, Geology
• 1996
Abstract We have already shown that a planet orbiting β Pictoris is able to confine the circumstellar dust. Here we present new numerical simulations which improve this model. The new model takes
A planetary system as the origin of structure in Fomalhaut's dust belt
• Physics, Geology
Nature
• 2005
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.