Formation of Protoplanet Systems and Diversity of Planetary Systems

By Eiichiro Kokubo, Shigeru Ida. 2002

340 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/c47c5b8af88990d438af668b823b32a59ea629a7

How researchers see this paper

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

In Astronomy and Astrophysics

Citations in the corpus

Formation of Hot Planets by a Combination of Planet Scattering, Tidal Circularization, and the Kozai Mechanism (2008, background): “In relativelymassive and/ormetal-rich disks,multiple gas giants are likely to form (e.g., Kokubo & Ida 2002; Ida & Lin 2004a, 2004b, 2008).”
Toward a Deterministic Model of Planetary Formation. IV. Effects of Type I Migration (2008, background): “Here, ‘‘cores’’ indicates the protoplanetary embryos that formed as a result of runaway or oligarchic growth of the accretion of planetesimals (Kokubo & Ida 1998, 2002).”
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).”
TEN NEW AND UPDATED MULTIPLANET SYSTEMS AND A SURVEY OF EXOPLANETARY SYSTEMS (2008, background): “Most planet formation theories are based on the core accretion model that begins with a disk of dust and gas where the dust particles collide and grow to form rock-ice planetary cores (Aarseth, Lin, & Palmer 1993; Kokubo & Ida 2002; Levison, Lissauer, & Duncan 1998).”
Post-oligarchic Evolution of Protoplanetary Embryos and the Stability of Planetary Systems (2007, methodology): “According to the numerical simulations of planet formation (Kokubo & Ida 2002, Ida & Lin 2004), after the planetary embryos have depleted nearby planetesimals and reached isolation masses, the embryos were separated with k0 ∼ 10− 12.”
MIGRATION THEN ASSEMBLY: FORMATION OF NEPTUNE-MASS PLANETS INSIDE 1 AU (2011, methodology): “In each case, we start with the surface density profile consisting of a series of protoplanetary embryos realized according to the oligarchic distribution described in Equations (17) and (18) of Kokubo & Ida (2002), spaced out between 0.05 AU to 1 AU.”
Oligarchic growth of giant planets (2003, background): “…assratio ofany two protoplanetsatadjacent locationsin the disk approachesunity overtim e. Ida and M akino (1993)investigated this transition analytically and through N-body sim ulations,and Kokubo and Ida (1998,2000, 2002)studied thesubsequentaccretion m ode,giving itthenam e\oligarchicgrowth".”
Dynamical Outcomes of Planet-Planet Scattering (2007, methodology): “According to the model of oligarchic growth, planetesimals form in a nearly maximally packed configuration in the protoplanetary disk, followed by gas accretion (Goldreich et al. 2004; Ida & Lin 2004b; Kokubo & Ida 2002).”
Extrasolar planet population synthesis I: Method, formation tracks and mass-distance distribution (2009, background): “During the early stages of planetary accretion, the process of embryo growth proceeds mainly by accumulation of background planetesimals and can be well described in the two-body approximation (Kokubo & Ida 2002).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS. II. EXTENSION TO FAINTER SOURCES (2010, background): “…should not adversely affect the likelihood of planet formation if sufficient mass is available, but it is expected to have an impact on the orbital architecture and migration properties of any resulting planetary system (Kokubo & Ida 2002; Chambers & Cassen 2002; Raymond et al. 2005; Crida 2009).”
MAKE SUPER-EARTHS, NOT JUPITERS: ACCRETING NEBULAR GAS ONTO SOLID CORES AT 0.1 AU AND BEYOND (2014, background): “Depletion factors are less severe if oligarchs are spaced by < 10 mutual 16 Hill radii (Kokubo & Ida 2000, 2002) and more severe if oligarchs’ initial inclinations and eccentricities are lower (Yoshinaga et al. 1999; Zhou et al. 2007).”
Water and astrobiology (2007, background): “Given that planetary embryos should form faster closer to the Sun (Kokubo and Ida, 2002), it is highly likely that Earth achieved the 10% of its final mass necessary to gravitationally capture nebular gases well within the lifetime of the Solar nebula.”
Predictions of the WFIRST Microlensing Survey. I. Bound Planet Detection Rates (2018, background): “…from high to low masses, characteristic mass scales include the critical core mass for runaway gas accretion at ∼10M⊕ (Mizuno 1980), the isolation mass of planetary embryos at ∼0.1M⊕ (Kokubo & Ida 2002), and the transition core mass for pebble accretion at ∼0.01M⊕ (Lambrechts & Johansen 2012).”
COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. I. OUTCOME REGIMES AND SCALING LAWS (2011, background): “For example, N -body simulations show that large (∼ 100 km) planetesimals may grow into protoplanets of about a lunar mass on million year time scales (e.g., Kokubo & Ida 2002).”
Toward a Deterministic Model of Planetary Formation. II. The Formation and Retention of Gas Giant Planets around Stars with a Range of Metallicities (2004, methodology): “Through gravitational interaction and coagulation, planetesimals evolve into cores through runaway (Greenberg et al. 1978; Wetherill & Stewart 1989; Aarseth et al. 1993; Kokubo & Ida 1996) and oligarchic growth (Kokubo & Ida 1998, 2002).”
Grain Retention and Formation of Planetesimals near the Snow Line in MRI-driven Turbulent Protoplanetary Disks (2007, methodology): “Kokubo & Ida 2002, Ida & Lin 2004, hereafter IL04), authors have often utilized an empirical “minimum mass nebula model” (MMNM) in which Σp ≃ 10r −3/2 AU g cm −2, where rAU is the radial distance from the central star.”