New Paradigms for Asteroid Formation

  title={New Paradigms for Asteroid Formation},
  author={Anders Johansen and Emmanuel Jacquet and Jeffrey N. Cuzzi and Alessandro Morbidelli and Matthieu Gounelle},
  journal={arXiv: Earth and Planetary Astrophysics},
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 population of initially km-scale planetesimals. However, new models challenge this idea by demonstrating that asteroids of sizes from 100 to 1000 km can form directly from the gravitational collapse of small particles which have organised themselves in dense filaments and clusters in the turbulent gas… 

Figures from this paper

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

Instabilities and Flow Structures in Protoplanetary Disks: Setting the Stage for Planetesimal Formation.

This chapter highlights the properties of turbulence and meso-scale flow structures in protoplanetary disks and their role in the planet formation process. Here we focus on the formation of

Dawes Review 7: The Tidal Downsizing Hypothesis of Planet Formation

  • S. Nayakshin
  • Physics, Geology
    Publications of the Astronomical Society of Australia
  • 2017
Abstract Tidal Downsizing scenario of planet formation builds on ideas proposed by Gerard Kuiper in 1951. Detailed simulations of self-gravitating discs, gas fragments, dust grain dynamics, and

The Compositional Structure of the Asteroid Belt

The past decade has brought major improvements in large-scale asteroid discovery and characterization with over half a million known asteroids and over 100,000 with some measurement of physical

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

Short-lived radioisotopes in meteorites from Galactic-scale correlated star formation

Abstract Meteoritic evidence shows that the Solar system at birth contained significant quantities of short-lived radioisotopes (SLRs) such as 60Fe and 26Al produced in supernova explosions and in

Rubble Pile Asteroids

  • K. Walsh
  • Geology, Physics
    Annual Review of Astronomy and Astrophysics
  • 2018
The moniker rubble pile is typically applied to all Solar System bodies >200 m and <∼10 km in diameter; in this size range, there is an abundance of evidence that nearly every object is bound

Origin and Evolution of Volatile-rich Asteroids

Volatile-rich asteroids represent the largest population, about 42% (DeMeo and Carry, 2014), of objects found between 2 and 3.5 AU. They encompass asteroids from the C complex that are believed to

Testing accretion mechanisms of the H chondrite parent body utilizing nucleosynthetic anomalies

Planetary bodies a few hundred kilometers in radii are the precursors to larger planets but it is unclear whether these bodies themselves formed very rapidly or accreted slowly over several millions



Rapid planetesimal formation in turbulent circumstellar disks

It is reported that boulders can undergo efficient gravitational collapse in locally overdense regions in the midplane of the disk, and it is found that gravitationally bound clusters form with masses comparable to dwarf planets and containing a distribution of boulder sizes.

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

Towards initial mass functions for asteroids and Kuiper Belt Objects

The multifaceted planetesimal formation process

Accumulation of dust and ice particles into planetesimals is an important step in the planet formation process. Planetesimals are the seeds of both terrestrial planets and the solid cores of gas and


Planet formation occurs within the gas- and dust-rich environments of protoplanetary disks. Observations of these objects show that the growth of primordial submicron-sized particles into larger

Grain Retention and Formation of Planetesimals near the Snow Line in MRI-driven Turbulent Protoplanetary Disks

The first challenge in the formation of both terrestrial planets and the cores of gas giants is the retention of grains in protoplanetary disks. In most regions of these disks, gas attains

The structure of protoplanetary discs around evolving young stars

The formation of planets with gaseous envelopes takes place in protoplanetary accretion discs on time scales of several million years. Small dust particles stick to each other to form pebbles,

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

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.

Turbulent Concentration of MM-Size Particles in the Protoplanetary Nebula: Scaled-Dependent Multiplier Functions

The initial accretion of primitive bodies (asteroids and TNOs) from freely-floating nebula particles remains problematic. Here we focus on the asteroids where constituent particle (read "chondrule")