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Thermal evolution of planetesimals during accretion

Icarus, 2017
cited By 2International audienceAlthough the mass distribution of planetesimals during the early stages of planetary formation has been discussed in various studies, this is not the case for their temperature distribution.
Yanick Ricard, David Bercovici, Francis Albarede   +2 more
exaly   +2 more sources

Impact disruption of primordial planetesimals [PDF]

Planetary and Space Science, 2013
It isusually assumed that 1-10-km  sized planetesimals are formed    through coagulation processes and     continue to agglomerate via pairwise mergers.
Parisi, Mirta Gabriela
exaly   +2 more sources

Small planetesimals in a massive disk formed Mars

Icarus, 2013
Mars is likely to be a planetary embryo formed through collisions with planetesimals, which can explain its small mass and rapid formation timescale obtained from 182Hf-182W chronometry.
Nicolas Dauphas
exaly   +2 more sources

Thermal evolution and differentiation of planetesimals and planetary embryos

Icarus, 2012
International audienceIn early Solar System during the runaway growth stage of planetary formation, the distribution of planetary bodies progressively evolved from a large number of planetesimals to a smaller number of objects with a few dominant embryos.
Yanick Ricard, Ondřej Sramek, Stéphane Labrosse   +2 more
exaly   +2 more sources

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Radial Migration of Planetesimals

Astrophysics and Space Science, 1994
Planetesimals 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
Neuhäuser, R., Feitzinger, J.
openaire   +2 more sources

The origin of the planetesimal theory

Origins of Life, 1977
T. C. Chamberlin suggested in 1897, on the basis of geological and climatological arguments, that the planets were formed by accretion of cold solid partices. With F. R. Moulton he developed convincing arguments against the Laplace nebular hypothesis and published a comprehensive 'planetesimal theory' of the origin of the solar system in 1905.
openaire   +2 more sources

On the Formation of Planetesimals

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
K. Hourigan, A. J. R. Prentice
openaire   +1 more source

Xenon fractionation in porous planetesimals

Geochimica et Cosmochimica Acta, 1990
The distinctively fractionated Xe on Mars and Earth may have its root in a common source from which both planets accreted. We begin with Ozima and Nakazawa's hypothesis that terrestrial Xe fractionation was caused by gravitational separation of adsorbed solar nebular gases inside large porous planetesimals.
K, Zahnle, J B, Pollack, J F, Kasting
openaire   +2 more sources

PLANETESIMALS HERE. PLANETESIMALS THERE. PLANETESIMALS EVERYWHERE

Geological Society of America Abstracts with Programs, 2020
Myriam Telus, Maggie A. Thompson, Johanna Teske   +2 more
openaire   +1 more source

Formation and Properties of Fluffy Planetesimals

Astrophysics and Space Science, 1994
A mechanism of accumulation of grains in the primordial solar nebula is described. This process produces porous, low density compressible aggregates. Compaction of the aggregates in a collision between them dissipates the kinetic energy of the collision and can result in efficient growth.
Bertram Donn, J. Mark Duva
openaire   +1 more source