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Contemporary formation of early Solar System planetesimals at two distinct radial locations
Nature Astronomy, 2021The formation of planetesimals is expected to occur via particle-gas instabilities that concentrate dust into self-gravitating clumps 1 – 3 . Triggering these instabilities requires the prior pile-up of dust in the protoplanetary disk 4 , 5 .
A. Morbidelli +6 more
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Planetesimals: Early differentiation and consequences for planets
, 2017Processes 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.
L. Elkins‐Tanton, B. Weiss
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Accretion of the earliest inner Solar System planetesimals beyond the water snowline
Nature AstronomyHow and where the first generation of inner Solar System planetesimals formed remains poorly understood. Potential formation regions are the silicate condensation line and water snowline of the solar protoplanetary disk. Whether the chemical compositions
D. Grewal +4 more
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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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Gravoturbulent planetesimal formation
Physica Scripta, 2008We present a new scenario for the rapid formation of planetesimals based on the combined effects of turbulence and gravity. While it was generally accepted that these two effects cancel each other out, we found their interaction to be extremely beneficial for the accumulation of larger objects bound by gravity.
H Klahr, A Johansen
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Degassing of early-formed planetesimals restricted water delivery to Earth
Nature, 2023M. Newcombe +8 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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PLANETESIMALS HERE. PLANETESIMALS THERE. PLANETESIMALS EVERYWHERE
Geological Society of America Abstracts with Programs, 2020Myriam Telus +2 more
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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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