Making More Terrestrial Planets

By J. Chambers. 2001

550 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/80dc61e6de86cae165f075565b5cfa97f3cfac70

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In Astronomy and Astrophysics

Citations in the corpus

Terrestrial Planet Formation. I. The Transition from Oligarchic Growth to Chaotic Growth (2005, background): “Chambers (2001) starts his calculations with lunar mass objects, instead of planetesimals.”
Spacing of Kepler Planets: Sculpting by Dynamical Instability (2015, background): “The orbital spacings between terrestrial planets are 9 wide, with K ∼ 30− 40.2 These values have been reproduced by a number of simulations where these planets conglomerate out of a sea of smaller bodies (e.g., Chambers 2001; Kokubo et al. 2006; O’Brien et al. 2006; Morishima et al. 2010).”
Final Stages of Planet Formation (2004, background): “Indeed, detailed N-body simulations of terrestrial planet formation by Chambers (2001) produce stable systems on a timescale similar to tcoag.”
Calcium-48 isotopic anomalies in bulk chondrites and achondrites: Evidence for a uniform isotopic reservoir in the inner protoplanetary disk (2014, background): “Simulations of chaotic growth indicate that terrestrial planets grew by the accretion of embryos formed at various heliocentric distances, so that the final planets should be isotopically distinct from any of the accreted embryos (Chambers, 2001; O’Brien et al., 2006).”
Terrestrial planet formation with strong dynamical friction (2006, methodology): “Previous numerical simulations of terrestrial planet accretion (e.g., Chambers and Wetherill, 1998; Agnor et al., 1999; Chambers, 2001; Raymond et al., 2004) treated systems that began with no more than ∼200 bodies.”
Equilibration in the aftermath of the lunar-forming giant impact (2007, background): “For example, the material that collects to form the Earth has significant contributions from regions interior to Mercury and exterior to Mars (Chambers, 2001).”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, background): “The classical model (Wetherill, 1996; Chambers and Wetherill, 1998; Chambers, 2001; Levison and Agnor, 2003; O’Brien et al., 2006; Raymond et al., 2006, 2009, 2014; Morishima et al., 2008, 2010; Fischer et al., 2014) proposes that the giant planets formed near their current locations and influenced…”
Decay of Planetary Debris Disks (2005, background): “The accretion end game is predicted to be dominated by a small number of collisions between large bodies (e.g., the early Earth and the impactor that caused formation of the Earth’s Moon) and may stretch over 100– 200 million years (Chambers 2001).”
THE Hf-W ISOTOPIC SYSTEM AND THE ORIGIN OF THE EARTH AND MOON (2005, methodology): “Computer simulations of this final stage of accretion have succeeded in producing systems containing 2–4 terrestrial planets between 0 and 2 AU from the Sun, with roughly circular and coplanar orbits (Wetherill 1992, Chambers & Wetherill 1998, Agnor et al. 1999, Chambers 2001).”
Making other earths: dynamical simulations of terrestrial planet formation and water delivery (2003, background): “This is not a new problem, as many authors (e.g. Chambers 2001, 2003) have had trouble matching the low eccentricities and inclinations in our solar system to numerically formed terrestrial planets, and is, as of yet, unsolved.”
Planet formation by coagulation: A focus on Uranus and Neptune (2004, background): “Nonetheless, N-body simulations can be useful for following the evolution of a few hundred bodies (Chambers 2001; Ida & Makino 1992; Kokubo & Ida 1996, 2000; Levison & Stewart 2001).”
Building Terrestrial Planets (2012, methodology): “The first simulations of the terrestrial planet accretion process using modern integration techniques (Agnor et al. 1999; Chambers 2001; Chambers & Wetherill 1998, 2001) used as initial conditions a set of a few tens of planetary embryos and produced planets on orbits that were systematically too…”
Atmospheres of Protoplanetary Cores: Critical Mass for Nucleated Instability (2004, background): “This ‘‘slow accretion’’ regimemay take place after cores have reached the isolation mass by oligarchic growth (Chambers 2001; Goldreich et al. 2004).”
THE RADIUS DISTRIBUTION OF PLANETS AROUND COOL STARS (2013, background): “…of the distribution, its explanation might be similar to our current understanding of the origins of the inner Solar System (Goldreich et al. 2004; Chambers 2001): a large number of isolation-mass protoplanets form quickly, and once the gas and planetesimal disk dissipates, a period of dynamical…”