The Edgeworth-Kuiper debris disk

Abstract

(Abridged) The Edgeworth-Kuiper belt with its presumed dusty debris is a natural reference for extrsolar debris disks. We employ a new algorithm to eliminate the inclination and the distance selection effects in the known TNO populations to derive expected parameters of the "true" EKB. Its estimated mass is M_EKB=0.12 M_earth, which is by a factor of \sim 15 larger than the mass of the EKB objects detected so far. About a half of the total EKB mass is in classical and resonant objects and another half is in scattered ones. Treating the debiased populations of EKB objects as dust parent bodies, we then "generate" their dust disk with our collisional code. Apart from accurate handling of collisions and direct radiation pressure, we include the Poynting-Robertson (P-R) drag, which cannot be ignored for the EKB dust disk. Outside the classical EKB, the radial profile of the optical depth approximately follows tau \sim r^-2 which is roughly intermediate between the slope predicted analytically for collision-dominated (r^-1.5) and transport-dominated (r^-2.5) disks. The cross section-dominating grain size still lies just above the blowout size (\sim 1...2 \microm), as it would without the P-R transport. However, if the EKB were by one order of magnitude less massive, the optical depth profile would fall off as tau \sim r^-3, and the cross section-dominating grain size would shift from \sim 1...2\microm to ~100 \microm. These properties are seen if dust is assumed to be generated only by known TNOs. If the solar system were observed from outside, the thermal emission flux from the EKB dust would be about two orders of magnitude lower than for solar-type stars with the brightest known infrared excesses observed from the same distance. Herschel and other new-generation facilities should reveal extrasolar debris disks nearly as tenuous as the EKB disk. The Herschel/PACS instrument should be able to detect disks at a \sim 1...2M_EKB level.

18 pages, 14 figures, accepted for publication in A&A

References in corpus (15)

• Spitzer IRS Spectroscopy of IRAS-Discovered Debris Disks
• Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 Solar Mass Main Sequence Stars
• Nearby debris disk systems with high fractional luminosity reconsidered
• New Debris Disks Around Nearby Main Sequence Stars: Impact on The Direct Detection of Planets
• Long-Term Collisional Evolution of Debris Disks
• Steady-State Size Distributions for Collisional Populations: Analytical Solution with Size-Dependent Strength
• Collisional processes and size distribution in spatially extended debris discs
• High Albedos of Low Inclination Classical Kuiper Belt Objects
• The Size Distribution of Kuiper belt objects for D> 10 km
• The History of the Solar System's Debris Disc: Observable Properties of the Kuiper Belt
• The Kuiper Belt Luminosity Function from m(R)=21 to 26
• Study of the Surface of 2003 EL61: the largest carbon-depleted object in the trans-neptunian belt
• Collisional and Thermal Emission Models of Debris Disks: Towards Planetesimal Population Properties
• A Possible Icy Kuiper Belt around HD 181327
• On the nature of clumps in debris disks

Cited by in corpus (33)

• DUst Around NEarby Stars. The survey observational results
• Resolved Debris Discs Around A Stars in the Herschel DEBRIS Survey
• Debris disk size distributions: steady state collisional evolution with P-R drag and other loss processes
• Herschel imaging of 61 Vir: implications for the prevalence of debris in low-mass planetary systems
• Stochastic accretion of planetesimals onto white dwarfs: constraints on the mass distribution of accreted material from atmospheric pollution
• Analysis of the Herschel DEBRIS Sun-like star sample
• Disk Radii and Grain Sizes in Herschel-Resolved Debris Disks
• A near-infrared interferometric survey of debris-disc stars. IV. An unbiased sample of 92 southern stars observed in H-band with VLTI/PIONIER
• An improved model of the Edgeworth-Kuiper debris disk
• Herschel's "Cold Debris Disks": Background Galaxies or Quiescent Rims of Planetary Systems?
• ALMA observations of the debris disk around the young Solar Analog HD 107146
• The cold origin of the warm dust around epsilon Eridani
• The Northern Arc of $\epsilon$ Eridani's Debris Ring as Seen by ALMA
• Collisional modelling of the AU Microscopii debris disc
• Cometary impactors on the TRAPPIST-1 planets can destroy all planetary atmospheres and rebuild secondary atmospheres on planets f, g, h
• Inner mean-motion resonances with eccentric planets: A possible origin for exozodiacal dust clouds
• Herschel discovery of a new class of cold, faint debris discs
• Near-infrared emission from sublimating dust in collisionally active debris disks
• Mass of the Kuiper Belt
• Fomalhaut b as a Dust Cloud: Frequent Collisions within the Fomalhaut Disk
• Observing planet-disk interaction in debris disks
• A peculiar class of debris disks from Herschel/DUNES - A steep fall off in the far infrared
• The Pseudo-zodi Problem for Edge-on Planetary Systems
• Will New Horizons see dust clumps in the Edgeworth-Kuiper belt?
• Grain Size segregation in debris discs
• The Transit Light Curve of an Exozodiacal Dust Cloud
• Forming the Cold Classical Kuiper Belt in a light Disk
• The Inner Debris Structure in the Fomalhaut Planetary System
• Astrophysics with New Horizons: Making the Most of a Generational Opportunity
• Absorption of crystalline water ice in the far infrared at different temperatures
• Calibration of the angular momenta of the minor planets in the solar system
• The Contribution of Dwarf Planets to the Origin of Low Inclination Comets by the Replenishment of Mean Motion Resonances in Debris Disks
• The Debiased Kuiper Belt: Our Solar System as a Debris Disk