A semi-analytic model for oligarchic growth

By J. Chambers. 2006

133 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/3f5944206ff61deef63928ba128db552e92fae49

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In Astronomy and Astrophysics

Citations in the corpus

Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 M☉ Main-Sequence Stars (2008, background): “Runaway growth ends; oligarchic growth begins (Kokubo & Ida 1998; Rafikov 2003; Chambers 2006; Nagasawa et al. 2007).”
Extrasolar planet population synthesis I: Method, formation tracks and mass-distance distribution (2009, methodology): “As initial values at t = 0, we use a mass of 0.66m3/5pla M 2/5 iso (Chambers 2006).”
Dynamics of pebbles in the vicinity of a growing planetary embryo: hydro-dynamical simulations (2012, background): “…∼10 Earth masses (ME) form beyond the so-called snowline (the orbital radius beyond which temperature is cold enough that water condenses into ice; Podolak & Zucker 2004), as required in the core-accretion model for giant planet formation (Thommes et al. 2003; Goldreich et al. 2004; Chambers 2006).”
Extrasolar planet population synthesis - II. Statistical comparison with observations (2009, methodology): “…as the accretion rate is the same for a migrating as for a non migrating planet, and we use a simple ∝ r−3/2 law for the solid surface density, which could be modified for example by planetesimal drift due to gas drag which occurs on the fastest timescales at small distances (e.g. Chambers 2006).”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, methodology): “, 2009, 2010) and viscous disk theory (Lynden-Bell and Pringle, 1974; Chambers, 2006; Bitsch et al., 2015) we chose a simple power-law profile for the disk.”
Building Terrestrial Planets (2012, background): “their mutual collisions rather become disruptive. Thus, the small bodies can only participate in the growth of the embryos. This phase is called `oligarchic growth' (Kokubo & Ida 1998, 2000, Chambers 2006). The runaway growth phase happens throughout the disk on a timescale that depends on ”
The effect of gas drag on the growth of protoplanets. Analytical expressions for the accretion of small bodies in laminar disks (2010, background): “…of the protoplanet and the central star, and αp the ratio between the protoplanet radius and the Hill radius, αp = Rp/Rh. Equation (1) is often used in statistical models for the accretion rate (e.g., Inaba et al. 2001; Chambers 2006; Brunini & Benvenuto 2008; Chambers 2008; Kobayashi et al. 2010).”
Debris disks as signposts of terrestrial planet formation (2011, background): “…that used in recent simulations of late-stage terrestrial accretion (Chambers 2001; Raymond et al. 2006a, 2009c; Morishima et al. 2010), but is within a factor of ∼2 of that obtained from semianalytic models of oligarchic growth (Chambers 2006) over the radial range between 1 AU and 3 AU at 3 Myr.”
Asteroids Were Born Big (2009, background): “In the outer Solar System, beyond the so-called snowline (Podolak and Zucker, 2004), it is generally expected that the end result is the formation of a few super-Earth cores (Thommes et al., 2003; Goldreich et al., 2004; Chambers, 2006) that, by accretion of a massive gaseous atmosphere from the dis”