Debris disks: seeing dust, thinking of planetesimals and planets

@article{Krivov2010DebrisDS,
  title={Debris disks: seeing dust, thinking of planetesimals and planets},
  author={Alexander V. Krivov},
  journal={Research in Astronomy and Astrophysics},
  year={2010},
  volume={10},
  pages={383-414}
}
  • A. Krivov
  • Published 26 March 2010
  • Physics, Geology
  • Research in Astronomy and Astrophysics
Debris disks are optically thin, almost gas-free dusty disks observed around a significant fraction of main-sequence stars older than about 10 Myr. Since the circumstellar dust is short-lived, the very existence of these disks is considered as evidence that dust-producing planetesimals are still present in mature systems, in which planets have formed - or failed to form - a long time ago. It is inferred that these planetesimals orbit their host stars at asteroid to Kuiper-belt distances and… 

Figures from this paper

Debris disks as signposts of terrestrial planet formation
There exists strong circumstantial evidence from their eccentric orbits that most of the known extra-solar planetary systems are the survivors of violent dynamical instabilities. Here we explore the
Debris disks as signposts of terrestrial planet formation - II. Dependence of exoplanet architectures on giant planet and disk properties
We present models for the formation of terrestrial planets, and the collisional evolution of debris disks, in planetary systems that contain multiple marginally unstable gas giants. We previousl y
Evolution of gas and dust in circumstellar environments: from protoplanetary discs to the formation of planets
Understanding the evolution of gas and dust in circumstellar discs is a major topic in present day astronomy, linked to one of the most interesting challenges: understanding the formation of planets.
Transient dust in warm debris disks - Detection of Fe-rich olivine grains
Context. Debris disks trace remnant reservoirs of leftover planetesimals in planetary systems. In the past years, a handful of “warm” debris disks have been discovered in which emission in excess
Dust spreading in debris discs: do small grains cling on to their birth environment?
Debris discs are dusty belts of planetesimals around main-sequence stars, similar to the asteroid and Kuiper belts in our Solar system. The planetesimals cannot be observed directly, yet they
Correlations between the stellar, planetary, and debris components of exoplanet systems observed byHerschel
Context. Stars form surrounded by gas- and dust-rich protoplanetary discs. Generally, these discs dissipate over a few (3–10) Myr, leaving a faint tenuous debris disc composed of second-generation
Dusty Planetary Systems
Extensive photometric stellar surveys show that many main sequence stars show emission at infrared and longer wavelengths that is in excess of the stellar photosphere; this emission is thought to
Observing planet-disk interaction in debris disks
Context. Structures in debris disks induced by planetdisk interaction are promising to provide valuable constraints on the existence and properties of embedded planets. Aims. We investigate the
Impact of planetesimal eccentricities and material strength on the appearance of eccentric debris disks
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
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
...
...

References

SHOWING 1-10 OF 207 REFERENCES
Evolution of Debris Disks
Circumstellar dust exists around several hundred main sequence stars. For the youngest stars, that dust could be a remnant of the protoplanetary disk. Mostly it is inferred to be continuously
ON THE RELATIONSHIP BETWEEN DEBRIS DISKS AND PLANETS
Dust in debris disks is generated by collisions among planetesimals. The existence of these planetesimals is a consequence of the planet formation process, but the relationship between debris disks
Extra-Solar Kuiper Belt Dust Disks
The dust disks observed around mature stars are evidence that plantesimals are present in these systems on spatial scales that are similar to that of the asteroids and the KBOs in the Solar System.
A Survey for Massive Giant Planets in Debris Disks with Evacuated Inner Cavities
The commonality of collisionally replenished debris around main-sequence stars suggests that minor bodies are frequent around Sun-like stars.Whether or not debris disks in general are accompanied by
A search for debris discs around stars with giant planets
Eight nearby stars with known giant planets have been searched for thermal emission in the submillimetre arising from dust debris. The null results imply quantities of dust typically less than 0.02
Metallicity, debris discs and planets
We investigate the populations of main-sequence stars within 25 pc that have debris discs and/or giant planets detected by Doppler shift. The metallicity distribution of the debris sample is a very
The total number of giant planets in debris discs with central clearings
Infrared spectra from the Spitzer Space Telescope (SSC) of many debris discs are well fit with a single blackbody temperature which suggest clearings within the disc. We assume that clearings are
Signatures of the Giant Planets Imprinted on the Edgeworth-Kuiper Belt Dust Disk
One method to detect extrasolar planetary systems is to deduce the perturbations of planets on the observed circumstellar dust disks. Our solar system, with its known configuration of planets,
Collisional and Thermal Emission Models of Debris Disks: Toward Planetesimal Population Properties
Debris disks around main-sequence stars are believed to derive from planetesimal populations that have accreted at early epochs and survived possible planet formation processes. While debris disks
COLLISIONAL CASCADES IN PLANETESIMAL DISKS. II. EMBEDDED PLANETS
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
...
...