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

@article{Krivov2020SolutionTT,
  title={Solution to the debris disc mass problem: planetesimals are born small?},
  author={Alexander V. Krivov and Mark C. Wyatt},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2020},
  volume={500},
  pages={718-735}
}
  • A. KrivovM. Wyatt
  • Published 17 August 2020
  • Geology, Physics
  • Monthly Notices of the Royal Astronomical Society
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 emission of dust released in collisions amongst directly unobservable larger bodies that carry most of the debris disc mass. We estimate the total mass of the discs by extrapolating up the mass of emitting dust with the help of collisional cascade models. The resulting mass of bright debris discs appears… 

The Mass Budgets and Spatial Scales of Exoplanet Systems and Protoplanetary Disks

Planets are born from disks of gas and dust, and observations of protoplanetary disks are used to constrain the initial conditions of planet formation. However, dust mass measurements of Class II

From Pebbles and Planetesimals to Planets and Dust: The Protoplanetary Disk–Debris Disk Connection

The similar orbital distances and detection rates of debris disks and the prominent rings observed in protoplanetary disks suggest a potential connection between these structures. We explore this

Formation of Gaps in Self-gravitating Debris Disks by Secular Resonance in a Single-planet System. I. A Simplified Model

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

Millimeter Dust Emission and Planetary Dynamics in the HD 106906 System

Debris disks are dusty, optically thin structures around main-sequence stars. HD 106906AB is a short-period stellar binary, host to a wide-separation planet, HD 106906b, and a debris disk. Only a few

Resolving the outer ring of HD 38206 using ALMA and constraining limits on planets in the system

HD 38206 is an A0V star in the Columba association, hosting a debris disc first discovered by IRAS. Further observations by Spitzer and Herschel showed that the disc has two components, likely

Survival of ALMA rings in the absence of pressure maxima

Recent ALMA observations have revealed that a large fraction of protoplanetary discs contain bright rings at (sub)millimeter wavelengths. Dust trapping induced by pressure maxima in the gas disc is a

Dust Resurgence in Protoplanetary Disks Due to Planetesimal–Planet Interactions

Observational data on the dust content of circumstellar disks show that the median dust content in disks around pre-main-sequence stars in nearby star-forming regions seems to increase from ∼1 to ∼2

Rapid formation of exoplanetesimals revealed by white dwarfs

The timing of formation for the first planetesimals determines the mode of planetary accretion and their geophysical and compositional evolution. Astronomical observations of circumstellar discs and

A ∼75 per cent occurrence rate of debris discs around F stars in the β Pic moving group

Only 20 per cent of old field stars have detectable debris discs, leaving open the question of what disc, if any, is present around the remaining 80 per cent. Young moving groups allow to probe

A molecular wind blows out of the Kuiper belt

Context. In this Letter we aim to explore whether gas is also expected in the Kuiper belt (KB) in our Solar System. Aims. To quantify the gas release in our Solar System, we use models for gas

References

SHOWING 1-10 OF 146 REFERENCES

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

Molecular Gas Clumps from the Destruction of Icy Bodies in the β Pictoris Debris Disk

A highly asymmetric disk of dust and carbon monoxide orbiting the planet-hosting star, β Pictoris, delineates a region of enhanced collisions, either from a mean motion resonance with an unseen giant planet or from the remnants of a collision of Mars-mass planets.

The Mass of Stirring Bodies in the AU Mic Debris Disk Inferred from Resolved Vertical Structure

The vertical distribution of dust in debris disks is sensitive to the number and size of large planetesimals dynamically stirring the disk, and is therefore well-suited for constraining the

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.

Debris disc stirring by secular perturbations from giant planets

Detectable debris discs are thought to require dynamical excitation (`stirring'), so that planetesimal collisions release large quantities of dust. We investigate the effects of the secular

Constraining the Solar System's Debris Disk with In Situ New Horizons Measurements from the Edgeworth–Kuiper Belt

The solar system currently possesses two remnant debris disks leftover from the planetary formation era in the form of the asteroid belt and the Edgeworth–Kuiper Belt (EKB). Similar to other stellar

Have protoplanetary discs formed planets

It has recently been noted that many discs around T Tauri stars appear to comprise only a few Jupiter masses of gas and dust. Using millimetre surveys of discs within six local star formation

Debris disc formation induced by planetary growth

Several hundred stars older than 10 million years have been observed to have infrared excesses. These observations are explained by dust grains formed by the collisional fragmentation of hidden

Collisional modelling of the AU Microscopii debris disc

The spatially resolved AU Mic debris disc is among the most famous and best-studied debris discs. We aim at a comprehensive understanding of the dust production and the dynamics of the disc objects

Stirring in massive, young debris discs from spatially resolved Herschel images

A significant fraction of main-sequence stars are encircled by dusty debris discs, where the short-lived dust particles are replenished through collisions between planetesimals. Most destructive
...