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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
Neuhäuser, R., Feitzinger, J.
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2017
Processes governing the evolution of planetesimals are critical to understanding how rocky planets are formed, how water is delivered to them, the origin of planetary atmospheres, how cores and magnetic dynamos develop, and ultimately, which planets have the potential to be habitable.
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Processes governing the evolution of planetesimals are critical to understanding how rocky planets are formed, how water is delivered to them, the origin of planetary atmospheres, how cores and magnetic dynamos develop, and ultimately, which planets have the potential to be habitable.
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The origin of the planetesimal theory
Origins of Life, 1977T. 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.
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On the Formation of Planetesimals
Publications of the Astronomical Society of Australia, 1979The 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
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PLANETESIMALS HERE. PLANETESIMALS THERE. PLANETESIMALS EVERYWHERE
Geological Society of America Abstracts with Programs, 2020Myriam Telus +2 more
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Xenon fractionation in porous planetesimals
Geochimica et Cosmochimica Acta, 1990The 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
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The Development of the Planetesimal Hypothesis
Science, 1909T C, Chamberlin, F R, Moulton
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Melt migration in rubble-pile planetesimals: Implications for the formation of primitive achondrites
Earth and Planetary Science Letters, 2023Zhongtian Zhang +2 more
exaly
Planetesimal Population Synthesis: are Planetesimals formed in Pressure Bumps?
2019Planetesimals, the smallest building blocks of planets that are gravitationally bound, are believed to be needed in order to form planets. The spacial distribution of these objects that are typically 100 km in diameter is important for the outcome of planet formation.
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