Formation of Protoplanets from Planetesimals in the Solar Nebula

By Eiichiro Kokubo, Shigeru Ida. 2000

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In Astronomy and Astrophysics

Citations in the corpus

On the ionisation fraction in protoplanetary disks. I. Comparing different reaction networks (2005, background): “The growth of planetesimals is controlled by the velocity dispersion (e.g. Wetherill & Stewart 1993), as is the growth of protoplanetary cores (Kokubo & Ida 2000; Thommes et al. 2003).”
The minimum-mass extrasolar nebula: in situ formation of close-in super-Earths (2012, background): “…predicts that an “oligarchy” composed of closely nested protoplanets eventually destabilizes when the oligarchs viscously stir themselves faster than the underlying disk can cool them by dynamical friction (e.g., Kokubo & Ida 2000; Goldreich et al. 2004; Kenyon & Bromley 2006; Ford & Chiang 2007).”
Toward a Deterministic Model of Planetary Formation. III. Mass Distribution of Short-Period Planets around Stars of Various Masses (2005, background): “…(Greenberg et al. 1978; Wetherill & Stewart 1989; Aarseth et al. 1993; Kokubo & Ida 1996), 3) oligarchic growth of protoplanetary embryos (Kokubo & Ida 1998, 2000), and 4) gas accretion onto solid cores (embryos) (Mizuno 1980; Bodenheimer & Pollack 1986; Pollack et al. 1996; Ikoma et al.…”
Three-dimensional Interaction between a Planet and an Isothermal Gaseous Disk. II. Eccentricity Waves and Bending Waves (2004, background): “However, inclinations and eccentricities of planets are thought to be smaller than the aspect ratio in the stage of planetary accretion (e.g., Wetherill & Stewart 1989; Kokubo & Ida 2000).”
Building Terrestrial Planets (2012, background): “This phase is termed oligarchic growth (Chambers 2006; Kokubo & Ida 1998, 2000).”
Making other earths: dynamical simulations of terrestrial planet formation and water delivery (2003, methodology): “Simulations of oligarchic growth by Kokubo & Ida (2000) suggest that planetary embryos form in < 1 Myr at 1 AU, in ∼40 Myr at 5 AU, and in > 300 Myr past 10 AU.”
Toward a Deterministic Model of Planetary Formation. I. A Desert in the Mass and Semimajor Axis Distributions of Extrasolar Planets (2003, background): “If the radial diffusion/migration of the cores is neglected, the isolation mass (Lissauer 1987; Kokubo & Ida 1998, 2000) Mc,iso = 2πa∆acΣd (19) represents the asymptotic mass of the cores prior to the depletion of the disk gas.”
The great dichotomy of the Solar System: Small terrestrial embryos and massive giant planet cores (2015, background): “By definition of ‘‘completion’’, the mass of the body is of the order of that originally available in an annulus around the orbit with a width equal to n times the Hill radius RH of the body itself, with n 10, independent of heliocentric distance (Kokubo and Ida, 2000).”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, background): “By the time of Jupiter’s gas accretion, the terrestrial region is thought to have been made up of roughly Mars-sized planetary embryos (Kokubo and Ida, 2000; Morbidelli et al., 2015) that presumably accreted predominantly from local, reduced material.”
THE Hf-W ISOTOPIC SYSTEM AND THE ORIGIN OF THE EARTH AND MOON (2005, background): “…the accretion process, when planetesimals with above average mass accreted material faster than smaller bodies and, eventually, the largest objects swept up most of the solid mass in the disk and became Moon- to Mars-sized planetary embryos (Kokubo & Ida 1998, 2000; Kortenkamp et al. 2000, 2001).”
Constraints on the Mass of a Habitable Planet with Water of Nebular Origin (2006, background): “After the runaway growth of protoplanets (Wetherill & Stewart 1993), they grow in an oligarchic fashion until they eat almost all of the planetesimals in their feeding zones (Kokubo & Ida 1998, 2000).”
The primordial excitation and clearing of the asteroid belt—Revisited (2006, background): “Finally, rather than assuming that all embryos are roughly Mars-mass, we could use a larger number of smaller embryos, or, as predicted by some embryo formation models (e.g., Kokubo and Ida, 2000), a distribution where embryo mass increases with distance from the Sun.”
THE COMPOSITIONAL DIVERSITY OF EXTRASOLAR TERRESTRIAL PLANETS. I. IN SITU SIMULATIONS (2010, background): “…the star and the giant planet (or in the case where there are one or more giant planets close to the host star such as 55Cnc and Gl777, in the region between the inner and outer giant planets) according to the relations between embryo mass, spacing, and orbital radius given by Kokubo & Ida (2000).”
Three-dimensional simulations of multiple protoplanets embedded in a protostellar disc (2008, methodology): “Numerical simulations of the oligarchic growth phase Article published by EDP Sciences have been used to examine the interactions of planetary embryos (Kokubo & Ida 2000; Thommes et al. 2003).”
The effect of gas drag on the growth of protoplanets. Analytical expressions for the accretion of small bodies in laminar disks (2010, background): “…(where most of the mass resides in leftover planetesimals) dynamical friction will keep the eccentricities of the most massive bodies small (e.g., Kokubo & Ida 2000); however, if most of the mass is transferred to the protoplanets their motion will become eccentric (see Kary & Lissauer 1995 for…”
MAKE SUPER-EARTHS, NOT JUPITERS: ACCRETING NEBULAR GAS ONTO SOLID CORES AT 0.1 AU AND BEYOND (2014, background): “The factor of ∼4 increase in solids from ice condensation raises oligarch masses by a factor of 43/2 to ∼5M⊕ at 5 AU within the minimum-mass solar nebula (MMSN; see, e.g., equation 22 of Kokubo & Ida 2000).”