Results 61 to 70 of about 21,167 (278)
Binary formation in planetesimal disks. II. Planetesimals with a mass spectrum [PDF]
Publications of the Astronomical Society of Japan, 2014 Abstract Many massive objects have been found in the outer region of the solar system. How they were formed and evolved has not been well understood, although there have been intensive studies of the accretion process of terrestrial planets. One of the mysteries is the existence of binary planetesimals with near-equal mass components and
Kominami, Junko D., Makino, Junichiro
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The Last Stages of Terrestrial Planet Formation: Dynamical Friction and the Late Veneer [PDF]
, 2012 The final stage of terrestrial planet formation consists of the cleanup of residual planetesimals after the giant impact phase. Dynamically, a residual planetesimal population is needed to damp the high eccentricities of the terrestrial planets after the
Albrecht +13 more
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A Long‐Lived Planetesimal Dynamo Powered by Core Crystallization
Geophysical Research Letters, 2021 The existence of numerous iron meteorite groups indicates that some planetesimals underwent melting that led to metal‐silicate segregation, sometimes producing metallic cores.
Clara Maurel +6 more
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Planetesimal Disk Evolution Driven by Planetesimal-Planetesimal Gravitational Scattering
The Astronomical Journal, 2003 29 pages, 1 figure, submitted to ...
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Wind-shearing in gaseous protoplanetary disks
, 2010 One of the first stages of planet formation is the growth of small planetesimals and their accumulation into large planetesimals and planetary embryos. This early stage occurs much before the dispersal of most of the gas from the protoplanetary disk. Due
Hagai B. Perets, Ormel, Ruth Murray-Clay
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Dust-to-gas ratio resurgence in circumstellar disks due to the formation of giant planets: the case of HD 163296 [PDF]
, 2019 The amount of dust present in circumstellar disks is expected to steadily decrease with age due to the growth from micron-sized particles to planetesimals and planets. Mature circumstellar disks, however, can be observed to contain significant amounts of
Marzari, F. +3 more
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, 2023 Review chapter of the book "Planetary Systems Now", to be published by World ...
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Self-stirring of debris discs by planetesimals formed by pebble concentration [PDF]
Monthly notices of the Royal Astronomical Society, 2018 When a protoplanetary disc loses gas, it leaves behind planets and one or more planetesimal belts. The belts get dynamically excited, either by planets ('planet stirring') or by embedded big planetesimals ('self-stirring').
A. Krivov, M. Booth
semanticscholar +1 more source
Life, 2014 The asteroid (4) Vesta, parent body of the Howardite-Eucrite-Diogenite meteorites, is one of the first bodies that formed, mostly from volatile-depleted material, in the Solar System. The Dawn mission recently provided evidence that hydrated material was
Diego Turrini, Vladimir Svetsov
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Planetesimal Initial Mass Functions Following Diffusion-regulated Gravitational Collapse
The Astrophysical Journal, 2023 The initial mass function (IMF) of planetesimals is of key importance for understanding the initial stages of planet formation, yet theoretical predictions so far have been insufficient in explaining the variety of IMFs found in simulations.
Konstantin Gerbig, Rixin Li
doaj +1 more source