Survivor Bias: Divergent Fates of the Solar System’s Ejected versus Persisting Planetesimals [PDF]
Astrophysical Journal, 2020 The orbital architecture of the solar system is thought to have been sculpted by a dynamical instability among the giant planets. During the instability a primordial outer disk of planetesimals was destabilized and ended up on planet-crossing orbits ...
S. Raymond +3 more
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Ice Sublimation in Planetesimals Formed at the Outward Migrating Snowline
The Astrophysical Journal Letters, 2023 Isotopic studies of meteorites suggest that planetesimals were formed as two distinct populations: noncarbonaceous (NC) and carbonaceous (CC) reservoirs.
Zhongtian Zhang
doaj +1 more source
PLANETARY MIGRATION IN EVOLVING PLANETESIMAL DISKS [PDF]
International Journal of Modern Physics D, 2003 In the current paper, we further improved the model for the migration of planets introduced and extended to time-dependent planetesimal accretion disks by Del Popolo. In the current study, the assumption of Del Popolo, that the surface density in planetesimals is proportional to that of gas, is relaxed. In order to obtain the evolution of planetesimal
İ. SAFFET YEŞİLYURT +2 more
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Pore Network Modeling of Core Forming Melts in Planetesimals
Frontiers in Earth Science, 2020 Early in the history of the solar system, planetesimals were differentiated into metallic cores. In some planetesimals, this differentiation took place by percolation of the denser core forming liquid through a lighter solid silicate matrix. A key factor
Giulio F. D. Solferino +2 more
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Planetesimal Growth in Evolving Protoplanetary Disks: Constraints from the Pebble Supply
The Astrophysical Journal, 2023 In the core accretion model, planetesimals grow by mutual collisions and engulfing millimeter-to-centimeter particles, i.e., pebbles. Pebble accretion can significantly increase the accretion efficiency and help explain the presence of planets on wide ...
Tong Fang +4 more
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Pebbles versus planetesimals [PDF]
, 2020 In the core accretion scenario, a massive core forms first and then accretes an envelope. When discussing how this core forms some divergences appear.
Natacha Brugger +4 more
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Testing the Jeans, Toomre, and Bonnor–Ebert Concepts for Planetesimal Formation: 3D Streaming-instability Simulations of Diffusion-regulated Formation of Planetesimals [PDF]
Astrophysical Journal, 2020 We perform streaming-instability simulations at Hill density and beyond to demonstrate that planetesimal formation is not completed when pebble accumulations exceed the local Hill density.
H. Klahr, A. Schreiber
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Planetesimal Population Synthesis: Pebble Flux-regulated Planetesimal Formation [PDF]
The Astrophysical Journal, 2019 Abstract We propose an expression for a local planetesimal formation rate proportional to the instantaneous radial pebble flux. The result—a radial planetesimal distribution—can be used as an initial condition to study the formation of planetary embryos.
Christian T. Lenz +2 more
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High-resolution Study of Planetesimal Formation by Gravitational Collapse of Pebble Clouds
The Astrophysical Journal, 2023 Planetary embryos are built through the collisional growth of 10–100 km-sized objects called planetesimals, a formerly large population of objects, of which asteroids, comets, and Kuiper Belt objects represent the leftovers from planet formation in our ...
Brooke Polak, Hubert Klahr
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Demographics of Planetesimals Formed by the Streaming Instability [PDF]
Astrophysical Journal, 2019 The streaming instability (SI) is a mechanism to aerodynamically concentrate solids in protoplanetary disks and facilitate the formation of planetesimals.
Rixin 新 Li 李日, A. Youdin, J. Simon
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