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On the Formation of Planetesimals [PDF]
Publications of the Astronomical Society of Australia, 1979 The past and present existence of smaller bodies in our solar system manifests itself in various ways through the appearance of asteroids, minor moons, planetary rings, surface cratering, etc. The occurrence of these planetesimals appears to be an integral intermediary step in the formation of the larger bodies from the initial grain state. In order to
A. J. R. Prentice, Kerry Hourigan
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Trans-Neptunian binaries as evidence for planetesimal formation by the streaming instability
Nature Astronomy, 2019A critical step toward the emergence of planets in a protoplanetary disk is the accretion of planetesimals, bodies 1–1,000 km in size, from smaller disk constituents.
D. Nesvorný +4 more
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Formation and Composition of Planetesimals
Space Science Reviews, 2005The composition of planetesimals depends upon the epoch and the location of their formation in the solar nebula. Meteorites produced in the hot inner nebula contain refractory compounds. Volatiles were present in icy planetesimals and cometesimals produced in the cold outer nebula.
Gautier, Daniel, Hersant, Franck
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Radial Migration of Planetesimals
Astrophysics and Space Science, 1994Planetesimals orbiting a protostar in a circumstellar disk are affected by gravitational interaction among themselves and by gas drag force due to disk gas. Within the Kyoto model of planetesimal accretion, the migration rate is interpreted as the inverse of the planetary formation time scale. Here, we study time scales of gravitational interaction and
J. V. Feitzinger, Ralph Neuhäuser
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American Mineralogist, 2020
The fourth installment of the evolutionary system of mineralogy considers two stages of planetesimal mineralogy that occurred early in the history of the solar nebula, commencing by 4.566 Ga and lasting for at least 5 million years: (1) primary igneous ...
S. Morrison, R. Hazen
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The fourth installment of the evolutionary system of mineralogy considers two stages of planetesimal mineralogy that occurred early in the history of the solar nebula, commencing by 4.566 Ga and lasting for at least 5 million years: (1) primary igneous ...
S. Morrison, R. Hazen
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Nature, 2017
In comparison to primitive, chondritic meteorites, which are widely thought to be the building blocks of Earth, Earth and other differentiated planetary bodies are chemically fractionated, with Earth's crust and mantlethe 'silicate Earth'being strongly depleted in moderately volatile elements (such as lead, zinc, indium and the alkali metals).
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In comparison to primitive, chondritic meteorites, which are widely thought to be the building blocks of Earth, Earth and other differentiated planetary bodies are chemically fractionated, with Earth's crust and mantlethe 'silicate Earth'being strongly depleted in moderately volatile elements (such as lead, zinc, indium and the alkali metals).
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Chronology of Planetesimal Differentiation
2017The differentiation of planetesimals from a loose aggregate of diverse solar nebula components into a compact and compositionally layered body consisting of core, mantle, and crust is one of the most fundamental processes in the early solar system. Differentiation involves the physical separation of metal and silicate through the segregation of dense ...
Kleine, T., Wadhwa, M.
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