Planetary accretion in the inner Solar System

By J. Chambers. 2004

340 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/84b113ceaff317b4af7cb38cb5927b7e2a2982fd

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In Astronomy and Astrophysics

Citations in the corpus

A Decreased Probability of Habitable Planet Formation around Low-Mass Stars (2007, background): “We assume that the disk evolved following the standard model of terrestrial planet growth (e.g. Chambers 2004): grains coalesced to form kmsized planetesimals; and embryos formed from planetes- imals via runaway and oligarchic growth (e.g., Kokubo & Ida 1998), spaced by 5-10 mutual Hill radii (RH,m…”
Building the terrestrial planets: Constrained accretion in the inner Solar System (2009, background): “ary Formation — Accretion — Origin, Solar System 1. INTRODUCTION It is commonly accepted that rocky planets form by the process of collisional agglomeration of smaller bodies (for recent reviews, see Chambers 2004, Nagasawa et al.2007 or Raymond 2008). This process starts from micron-sized dust grai”
Magma oceans in the inner solar system (2012, background): “Planetesimals of this size are expected to accrete on a timescale of 105 years (Goldreich & Ward 1973; see also recent reviews in Chambers 2004 and Canup 2008).”
Equilibration in the aftermath of the lunar-forming giant impact (2007, background): “Present scenarios of planet formation suggest that the process occurs in three stages: the growth of dust grains in the preplanetary disk into kilometer-sized planetesimals, the runaway growth of these planetesimals into lunar- to Mars-sized planetary embryos, and the final accretion of the planets ”
COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. II. THE DIVERSITY OF IMPACT OUTCOMES DURING THE END STAGE OF PLANET FORMATION (2011, background): “The end stage of terrestrial planet formation is defined by the final competition between planetary embryos as they grow via collisions into a final set of stable planets (e.g., Chambers 2004).”
Chondrule formation during planetesimal accretion (2011, background): “This led to random velocities φ ~ 1 associated with the heyday of oligarchic growth (Kokubo and Ida, 1998) and the giant impact phase of terrestrial planet formation (Chambers, 2004).”
Water and astrobiology (2007, background): “Numerical models that replicate planetary accretion in the inner Solar System (Morbidelli et al., 2000; Chambers, 2004; Raymond et al., 2004), from Mercury at 0.”
Melting and differentiation of early-formed asteroids: The perspective from high precision oxygen isotope studies (2017, background): “The Howardite, Eucrite, Diogenite suite (HEDs) is the most abundant group of differentiated meteorites arriving on Earth today, comprising roughly 6% of all witnessed falls (statistics from Mete- oritical Bulletin Database; see also Burbine et al., 2002a).”
Oxygen isotope constraints on the origin and differentiation of the Moon (2007, background): “In themost recent dynamical models for planetary accretion [62,68], the reduction of isotopic heterogeneity is a natural consequence of stochastic interaction and collision of increasingly larger planetary embryos, whereas smaller bodies may retain more of their initial isotopic variability.”
Towards initial mass functions for asteroids and Kuiper Belt Objects (2010, methodology): “Indeed Chambers (2010) has assumed an even smaller timescale for tpa, comparable to the (shorter) eddy timescale at lengthscale l << L.”
Emergence of a Habitable Planet (2007, background): “Runaway growth of the first generation planets is thought to have taken no more than 1 Myr (Lissauer 1993; Chambers 2004).”
Decay of Planetary Debris Disks (2005, background): “For example, the behavior might correlate with current ideas for the evolution of the solar system (e.g., Chambers 2004), where there is a period of 100–200 Myr when large, planet-sized bodies occasionally collide, followed by continued collisions between asteroid-sized objects.”
Terrestrial planet formation with strong dynamical friction (2006, background): “The accretion of the terrestrial planets in our Solar System has been the subject of much study, yet is far from being completely understood (see Chambers, 2004, for a recent and thorough review of the field).”
NEW DEBRIS DISKS AROUND YOUNG, LOW-MASS STARS DISCOVERED WITH THE SPITZER SPACE TELESCOPE (2009, neutral): “A second hypothesis is that the “bright disk stars” are undergoing an epoch of en- hanced planetesimal collisions akin to the Late Heavy Bombardment within our own Solar System when it was ∼700 Myr old (Kleine et al. 2002; Chambers 2004; Gomes et al. 2005; Strom et al. 2005).”