Coagulation Calculations of Icy Planet Formation at 15--150 AU: A Correlation Between the Maximum Radius and the Slope of the Size Distribution for Transneptunian Objects

Abstract

We investigate whether coagulation models of planet formation can explain the observed size distributions of transneptunian objects (TNOs). Analyzing published and new calculations, we demonstrate robust relations between the size of the largest object and the slope of the size distribution for sizes 0.1 km and larger. These relations yield clear, testable predictions for TNOs and other icy objects throughout the solar system. Applying our results to existing observations, we show that a broad range of initial disk masses, planetesimal sizes, and fragmentation parameters can explain the data. Adding dynamical constraints on the initial semimajor axis of `hot' KBOs along with probable TNO formation times of 10-700 Myr restricts the viable models to those with a massive disk composed of relatively small (1-10 km) planetesimals.

Text: 44 pages, Tables: 5, Figures: 17; Accepted for publication in the Astronomical Journal

References in corpus (19)

• Gas- and dust evolution in protoplanetary disks
• Planet formation around stars of various masses: The snow line and the frequency of giant planets
• Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune
• Toward a Deterministic Model of Planetary Formation V. Accumulation Near the Ice Line
• The Canada-France Ecliptic Plane Survey - Full Data Release: The orbital structure of the Kuiper belt
• Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 Solar Mass Main Sequence Stars
• Steady-State Size Distributions for Collisional Populations: Analytical Solution with Size-Dependent Strength
• Full Numerical Simulations of Catastrophic Small Body Collisions
• Evidence for Two Populations of Classical Transneptunian Objects: The Strong Inclination Dependence of Classical Binaries
• High Albedos of Low Inclination Classical Kuiper Belt Objects
• The Size Distribution of Kuiper belt objects for D> 10 km
• The Kuiper Belt Luminosity Function from m(R)=21 to 26
• A Hybrid N-body--Coagulation Code for Planet Formation
• Instability-Driven Dynamical Evolution Model of a Primordially 5 Planet Outer Solar System
• Rapid Formation of Icy Super-Earths and the Cores of Gas Giant Planets
• Coupling dynamical and collisional evolution of small bodies II : Forming the Kuiper Belt, the Scattered Disk and the Oort Cloud
• Color-Inclination Relation of the Classical Kuiper Belt Objects
• Mutual Orbits and Masses of Six Transneptunian Binaries
• Dynamically Excited Outer Solar System Objects in the Hubble Space Telescope Archive

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• Making Planet Nine: Pebble Accretion at 250--750 AU in a Gravitationally Unstable Ring
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• Coagulation Calculations of Icy Planet Formation Around 0.1--0.5~\msun\ Stars: Super-Earths From Large Planetestimals
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• Constructing a refined model of small bodies in the solar system - I. The Jovian Trojans
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