Formation of Giant Planets: Dependences on Core Accretion Rate and Grain Opacity

By M. Ikoma, K. Nakazawa, H. Emori. 2000

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In Astronomy and Astrophysics

Citations in the corpus

A FRAMEWORK FOR CHARACTERIZING THE ATMOSPHERES OF LOW-MASS LOW-DENSITY TRANSITING PLANETS (2013, background): “This is a consequence of the following: these very low mass planets can only accrete tenuous H/He envelopes since the gas accretion timescale nonlinearly (A color version of this figure is available in the online journal.) increases for lower core mass (e.g., Ikoma et al. 2000).”
Toward a Deterministic Model of Planetary Formation. II. The Formation and Retention of Gas Giant Planets around Stars with a Range of Metallicities (2004, background): “…be interpreted as evidence that the formation probability of gas giant planets is greatly enhanced in metal-rich protostellar disks, in accordance with the core-accretion scenario for formation of giant planets (e.g., Mizuno 1980; Bodenheimer & Pollack 1986; Pollack et al. 1996; Ikoma et al. 2000).”
IN SITU FORMATION AND DYNAMICAL EVOLUTION OF HOT JUPITER SYSTEMS (2015, background): “For example, envelope heating by planetesimal accretion could significantly prolong the phase of hydrostatic growth (Ikoma et al. 2000), rendering our estimate of the critical core mass an effective lower bound.”
The great dichotomy of the Solar System: Small terrestrial embryos and massive giant planet cores (2015, background): “…mass for the runaway accretion of the atmosphere depends on the rate at which the core accretes solids, on the molecular weight of the atmosphere (Ikoma et al., 2000; Hori and Ikoma, 2011) and the dust opacity in the envelope (Mizuno, 1980, Stevenson, 1982), which remains poorly known despite…”
Internal structure of massive terrestrial planets (2005, background): “Current simpler numeri al models (Ikoma et al. 2000) nd a robust dependen e on the rate of a retion, Ṁ , and the opa ity, κ, of the disk gas: Mcrit ⋍ 10 ( Ṁ 10−6M⊕yr−1 )q( κ 1cm2g−1 )s M⊕, where q and s lie between 0.2 and 0.3.”
MAKE SUPER-EARTHS, NOT JUPITERS: ACCRETING NEBULAR GAS ONTO SOLID CORES AT 0.1 AU AND BEYOND (2014, background): “Both Ikoma et al. (2000) and Papaloizou & Nelson (2005) conclude that Jupiter could have formed in-situ as long as Mcore & 5M⊕.”
Formation of Protoplanet Systems and Diversity of Planetary Systems (2002, background): “Conditions for Gas Giant Planet Formation Gas accretion begins when the growth timescale of a protoplanet becomes longer than the contraction timescale of the planetary atmosphere (Ikoma et al. 2000).”
Models of Jupiter's growth incorporating thermal and hydrodynamic constraints (2008, methodology): “Previous models of this process have simulated either the thermal factors that limit the ability of a planet to retain gas (Bodenheimer and Pollack 1986, hereafter BP86; Pollack et al. 1996, hereafter PHBLPG96; Bodenheimer et al. 2000, hereafter BHL00; Ikoma et al. 2000; Hubickyj et al. 2005, hereaf”
Origin and evolution of the atmospheres of early Venus, Earth and Mars (2018, background): “5MEarth, gravitational energy, short-lived radioactive elements together with captured H2-envelopes enhance the temperature of the planetary surface to ≥2000 K, resulting in deep global magma oceans (e.g., Mizuno et al. 1980; Mizuno and Wetherill 1984; Sasaki and Nakazawa 1989; Ikoma et al. 2000; Ik”
Formation of Jupiter using opacities based on detailed grain physics (2010, background): “One example is the (statistical + N-body) calculation of Inaba et al. (2003) which takes into account planetesimal fragmentation as well as the effect of the gaseous envelope in increasing the effective cross-section.”
TOWARD A DETERMINISTIC MODEL OF PLANETARY FORMATION. VI. DYNAMICAL INTERACTION AND COAGULATION OF MULTIPLE ROCKY EMBRYOS AND SUPER-EARTH SYSTEMS AROUND SOLAR-TYPE STARS (2010, background): “For solar composition gas, the critical core mass to hydrodynamically sustain the gas envelope is Mc,hydro ∼ 10 M⊕ (Mizuno 1980; Pollack et al. 1996; Ikoma et al. 2000).”
Atmospheres of Protoplanetary Cores: Critical Mass for Nucleated Instability (2004, methodology): “Our use of a simple power-law opacity in equation (10) may seem an oversimplification compared to other treatments (e.g., Mizuno 1980; Ikoma et al. 2000) employing realistic opacity tables.”
Toward a Deterministic Model of Planetary Formation. I. A Desert in the Mass and Semimajor Axis Distributions of Extrasolar Planets (2003, background): “Faster accretion and higher opacity (relatively large Ṁc and κ) result in a warmer planetary atmosphere and the enhanced pressure gradient stalls the gas accretion (Stevenson 1982; Ikoma et al. 2000).”
THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, background): “This core growth is accelerated for disks with higher densities (∝ Md; e.g., Ikoma et al. 2000; Hubickyj et al. 2005; Thommes et al. 2008), and sees modest benefits from shorter orbital periods (∝ √ M∗ at a fixed semimajor axis) and larger potential formation zones (∼ M∗; e.g., Kennedy & Kenyon…”
Planetesimal formation starts at the snow line (2017, background): “It is known that enhancement of about 10 times over the solids surface density corresponding to the minimum mass solar nebula is necessary to allow for Jupiter core formation before the gas disk dispersal (Pollack et al. 1996; Ikoma et al. 2000; Kobayashi et al. 2010).”
Planetary Torques as the Viscosity of Protoplanetary Disks (2000, background): “…expect that Zp is comparable to the metallicity of the gas if planet-formation is efficient but the planets are too small to have captured massive gaseous envelopes (Mizuno et al. 1978; Podolak et al. 1993; Ikoma et al. 2000) Then the average number of planets per unit radius is N = 2πrZpΣ 〈Mp〉 .”