Formation of Planetesimals and Accretion of the Terrestrial Planets

By S. Weidenschilling. 2000

134 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/f333894b12f201d0a4bf8f9af6d53cb8cee65613

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

Citations in the corpus

Material Enhancement in Protoplanetary Nebulae by Particle Drift through Evaporation Fronts (2004, background): “Detailed models of incremental growth, with realistic sticking and erosion based on laboratory experiments, tend to quickly produce broad power-law size distributions that contain equal mass per decade of particle radius (Weidenschilling 1997, 2000).”
Clumps in the outer disk by disk instability: Why they are initially gas giants and the legacy of disruption (2009, background): “However, there could have been substantial grain growth during this time, as meter-sized objects can grow in ∼ 1000 yr for the conditions in the clump (e,g, Weidenschilling, 2000).”
Early crust on top of the Earth''s core: Physics of the Earth and Planetary Interiors (2005, background): “During the post-great-collision stage, which may have lasted tens of millions of years, interactions with smaller bodies dominated (Angor et al., 1999; Weidenschilling, 2000).”
Towards initial mass functions for asteroids and Kuiper Belt Objects (2010, background): “If the nebula were nonturbulent, as required for traditional midplane instabilities to play a role, particles settle into a dense midplane layer and growth by incremental accretion comes to completion too quickly - numerous 100km planetesimals and even lunar-size objects form in 10(5) years (Weidens”
The hazard of near-Earth asteroid impacts on earth (2004, background): “There is scientific consensus that the planets grew, in part, from the accumulation of much smaller objects called ‘‘planetesimals’’ [2].”
Chondrule size and related physical properties: a compilation and evaluation of current data across all meteorite groups (2014, background): “ps could be a result of their mechanism of formation, a result of post-solidification nebular sorting, the result of a process on the parent body, or a combination of factors (e.g., Shu et al., 1996; Weidenschilling, 2000; Cuzzi et al., 2001; Cuzzi and Weidenschilling, 2006; Chiang and Youdin, 2010;”
Turbulent Mixing of Metal and Silicate during Planet Accretion – and interpretation of the Hf-W chronometer (2010, background): “01 m, which 2) clump together by turbulent motion to produce ∼1 km bodies (Weidenschilling, 2000).”
The fossilized size distribution of the main asteroid belt (2003, background): “…and the dynamical excitation of small b populations not yet accreted by the embryos (e.g.,Safronov, 1969; Greenberg et al., 1978; Wetherill and Stewart, 19 Weidenschilling et al., 1997; Chambers and Wetherill, 19 Agnor et al., 1999; Weidenschilling, 2000; Petit et al., 20 Kokubo and Ida, 2002).”
Ceres’ evolution and present state constrained by shape data (2010, background): “It is thought that, in the sequence of accretion from the Solar nebula, the terrestrial planets were formed from this class of objects (e.g., Canup and Agnor, 2000; Weidenschilling, 2006), but today only these three remain in the inner Solar System.”
The evolution of the water distribution in a viscous protoplanetary disk (2005, background): “Weidenschilling, 1980, 1984, 1997, 2000; Weidenschilling and Cuzzi, 1993; Dullemond and Dominik, 2005) have shown that a range of particle sizes would exist at a given location in the nebula.”