Towards initial mass functions for asteroids and Kuiper Belt Objects

  title={Towards initial mass functions for asteroids and Kuiper Belt Objects},
  author={Jeffrey N. Cuzzi and Robert C. Hogan and William F. Bottke},

Figures from this paper

New Paradigms for Asteroid Formation

Asteroids and meteorites provide key evidence on the formation of planetesimals in the Solar System. Asteroids are traditionally thought to form in a bottom-up process by coagulation within a

Growth of asteroids, planetary embryos, and Kuiper belt objects by chondrule accretion

It is shown that the main growth of asteroids can result from gas drag–assisted accretion of chondrules, and planetesimal accretion and chondrule accretion play more equal roles in the formation of Moon-sized embryos in the terrestrial planet formation region.

Accretion of the asteroids: Implications for their thermal evolution

Thermal models of asteroids generally assume that they accreted either instantaneously or over an extended interval with a prescribed growth rate. It is conventionally assumed that the onset of

Debris disc constraints on planetesimal formation

Two basic routes for planetesimal formation have been proposed over the last decades. One is a classical 'slow-growth' scenario. Another one is particle concentration models, in which small pebbles

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


The asteroid belt is an open window on the history of the solar system, as it preserves records of both its formation process and its secular evolution. The progenitors of the present-day asteroids

Geophysical evidence that Saturn’s Moon Phoebe originated from a C-type asteroid reservoir

Saturn’s Moon Phoebe has been suggested to originate from the Kuiper Belt. However, its density is twice that of Kuiper Belt objects (KBOs) in the same size class, which challenges that

Particle size distributions in chondritic meteorites: Evidence for pre-planetesimal histories

Cascade Model for Planetesimal Formation by Turbulent Clustering

We use a newly developed cascade model of turbulent concentration of particles in protoplanetary nebulae to calculate several properties of interest to the formation of primitive planetesimals and to



Were Asteroids Born Big? An Alternative Scenario

Introduction: Although most evidence for the size(s) of initial planetesimals has been destroyed, some evidence may be preserved in the asteroid belt. The size frequency distribution (SFD) in the

Toward Planetesimals: Dense Chondrule Clumps in the Protoplanetary Nebula

We outline a scenario that traces a direct path from freely floating nebula particles to the first 10-100 km sized bodies in the terrestrial planet region, producing planetesimals that have

Astronomical constraints on nebular temperatures: Implications for planetesimal formation

Abstract— Motivated by recent observations of T‐Tauri stars and the interpretation of these observations in terms of the properties of circumstellar disks, we derive internal (midplane) temperatures

Planet Formation in the Outer Solar System

This paper reviews coagulation models for planet formation in the Kuiper belt, emphasizing links to recent observations of our and other solar systems. At heliocentric distances of 35–50 AU,

Iron meteorites as remnants of planetesimals formed in the terrestrial planet region

It is shown that the iron-meteorite parent bodies most probably formed in the terrestrial planet region, and it is predicted that some asteroids are main-belt interlopers and a select few may even be remnants of the long-lost precursor material that formed the Earth.

Planetary accretion in the inner Solar System

The fossilized size distribution of the main asteroid belt

Planetesimal formation by turbulent concentration .

Ron Ballouz October 10,2012 Planets originate from a circumstellar protoplanetary disk made up of the remains of the stellar accretion disk. While most of this material is made up of Hydrogen and

Particle-Gas Dynamics and Primary Accretion

Abstract. Planetesinial bow shocks would have existed during the chondrule forniation epoch if proto-.Jupiter formed within a few Myr of CAI forniation and if the protoplanetary nebula persisted for