The taxonomy of planetesimals

Consequences for planets

Research output: Chapter in Book/Report/Conference proceedingChapter

Abstract

Introduction In past decades, planetary differentiation was posited to be a simple three-step process: accretion, core formation, and melting to form a crust. Now we know that differentiation is a far more complex process, that it occurred in very small early bodies long before completion of rocky planet formation, and that it has a variety of partial end-states. Iron meteorites demonstrate the existence of differentiated planetesimals in the first 500 000 years after solids formed in the disk (Scherstén et al., 2006), and (4) Vesta has differentiated into a metal core and silicate mantle (Raymond et al., Chapter 15, this volume). Johansen et al. (2015) suggest the icy asteroids formed 2 to 4 Myr after calcium-aluminum-rich inclusions (CAIs) (Castillo-Rogez and Young, Chapter 5, this volume). The breakthrough of pebble accretion, which shows that pebble-sized objects accrete to larger objects extremely efficiently through gravitational perturbation of their orbits, indicates that accretion timescale could have been as short as a few thousand years for 100-km-diameter objects (Johansen et al., 2014). This extremely short timescale supports the use of simple models that assume nearly instantaneous accretion relative to the timescale of 26Al heating, though pebble accretion would have continued past the point of 26Al activity, and coated the young planetesimals with unmelted rinds (A. Johansen, 2016, personal communication). Processes of Differentiation in Planetesimals All processes of differentiation begin with heating. Heating in planetesimals is the result of decay of 26Al (Urey, 1955); impacts are inefficient at raising temperature globally in such small and porous bodies. Models indicate that heating may have been rapid and extreme (Hevey and Sanders, 2006), but heating is moderated by 26Al content (Krot et al., 2012), ice content (Castillo-Rogez and McCord, 2010), and by the rate of accretion (see Castillo-Rogez and Young, Chapter 5, this volume). Metallic core formation relies on the ability of the separated, small metal blebs in the primitive material to flow together and downward in the small gravity field of the planetesimals. The Fe-FeS eutectic occurs at 31 wt% sulfur (equivalent to 85% FeS and 15% Fe) and at a temperature of 988 °C (Brett and Bell, 1969).

Original languageEnglish (US)
Title of host publicationPlanetesimals
Subtitle of host publicationEarly Differentiation and Consequences for Planets
PublisherCambridge University Press
Pages365-375
Number of pages11
ISBN (Electronic)9781316339794
ISBN (Print)9781107118485
DOIs
StatePublished - Jan 1 2017

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taxonomy
protoplanets
planets
heating
iron meteorites
asteroids
bells
eutectics
metals
calcium
silicates
crusts
Earth mantle
ice
sulfur
communication
melting
inclusions
gravitation
aluminum

ASJC Scopus subject areas

  • Physics and Astronomy(all)

Cite this

Elkins-Tanton, L. (2017). The taxonomy of planetesimals: Consequences for planets. In Planetesimals: Early Differentiation and Consequences for Planets (pp. 365-375). Cambridge University Press. https://doi.org/10.1017/9781316339794.017

The taxonomy of planetesimals : Consequences for planets. / Elkins-Tanton, Linda.

Planetesimals: Early Differentiation and Consequences for Planets. Cambridge University Press, 2017. p. 365-375.

Research output: Chapter in Book/Report/Conference proceedingChapter

Elkins-Tanton, L 2017, The taxonomy of planetesimals: Consequences for planets. in Planetesimals: Early Differentiation and Consequences for Planets. Cambridge University Press, pp. 365-375. https://doi.org/10.1017/9781316339794.017
Elkins-Tanton L. The taxonomy of planetesimals: Consequences for planets. In Planetesimals: Early Differentiation and Consequences for Planets. Cambridge University Press. 2017. p. 365-375 https://doi.org/10.1017/9781316339794.017
Elkins-Tanton, Linda. / The taxonomy of planetesimals : Consequences for planets. Planetesimals: Early Differentiation and Consequences for Planets. Cambridge University Press, 2017. pp. 365-375
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