Results 61 to 70 of about 832 (184)
Astronomy & AstrophysicsThe streaming instability and pebble accretion are two physical mechanisms with demonstrated potentials to drive, respectively, the formation of planetesimals and the growth of planetary systems containing a diverse range of planetary types.
Johansen Anders, Lyra Wladimir
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Collisions of Planetesimals and Formation of Planets [PDF]
Proceedings of the International Astronomical Union, 2015 AbstractWe present preliminary results of models of terrestrial planet formation using on the one hand classical numerical integration of hundreds of small bodies on CPUs and on the other hand—for comparison—the results of our GPU code with thousands of small bodies which then merge to larger ones.
Dvorak, Rudolf +5 more
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Surface Geology and Evolution of Asteroid Ryugu: Insights From Hayabusa2 Global Mapping
Journal of Geophysical Research: Planets, Volume 131, Issue 7, July 2026.Abstract Rubble‐pile asteroids, characterized by loose aggregates of debris held together by gravity, represent both a significant planetary hazard and a key to understanding planetesimal formation. Geologic mapping of these bodies provides essential insights into their origins, evolution, and surface processes.
Lisa M. Vincent +8 more
wiley +1 more source
WATER FRACTIONS IN EXTRASOLAR PLANETESIMALS [PDF]
The Astronomical Journal, 2011 Accepted for publication in the Astronomical Journal, 22 pages, 4 figures, 1 ...
Jura, M., Xu, S.
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Geochemistry, Geophysics, Geosystems, Volume 27, Issue 7, July 2026.Abstract Sulfur (S) is one of the promising light elements that can explain the density deficit of the core. The degree of siderophile nature of S under high pressure and temperature (P,T) is the key to estimating the S content in the core. However, a significant discrepancy between the metal‐silicate partition coefficient of S extrapolated from ...
K. Itoh, T. Tsuchiya
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From planetesimals to planets with N-body simulations in the giant-planet formation region
Astronomy & AstrophysicsThe cores of wide-orbit giant planets can form via pebble accretion if large planetesimals form in the outer regions of protoplanetary discs at sufficiently early times.
Lorek Sebastian, Lambrechts Michiel
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Widespread Impact‐Induced Crustal Permeability on the Early Earth
AGU Advances, Volume 7, Issue 3, June 2026.Abstract The early Earth (i.e., Archean and Hadean Eons, 2.5–4.0 and 4.0–4.5 Ga, respectively) experienced frequent cosmic bombardment. Impacts have been shown to stimulate crustal alteration, for instance via hydrothermal systems active for up to millions of years post‐impact.
A. M. Alexander +2 more
wiley +1 more source
Marc Chaussidon—Leonard Medal 2026
Meteoritics &Planetary Science, EarlyView.
François Robert
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Lunar Crustal Formation by Melt Migration and Differentiation Within a Stagnant Lid
Journal of Geophysical Research: Planets, Volume 131, Issue 6, June 2026.Abstract The lunar anorthosite highlands represent the Moon's primary crust, which formed during the solidification of a magma ocean following the Moon‐forming giant impact. However, the canonical model of anorthite flotation in the crystallizing magma ocean often struggles to reproduce the long > ${ >} $200 Myr solidification timescale required by the
K. H. Dodds, C. Michaut, J. A. Neufeld
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Terrestrial Planet Formation from Two Source Reservoirs
The Astronomical JournalThis work describes new dynamical simulations of terrestrial planet formation. The simulations started at the protoplanetary disk stage, when planetesimals formed and accreted into protoplanets, and continued past the late stage of giant impacts.
David Nesvorný +4 more
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