Accretion of the gaseous envelope of Jupiter around a 5–10 Earth-mass core

By O. Hubickyj, P. Bodenheimer, Jack J. Lissauer. 2005

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View Paper: https://www.semanticscholar.org/paper/e06586125e1ee52df7e86559a5ef129b6c85cb54

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In Astronomy and Astrophysics

Citations in the corpus

IN SITU FORMATION AND DYNAMICAL EVOLUTION OF HOT JUPITER SYSTEMS (2015, methodology): “= 1M and adopt a nebular temperature of 1500K (for full details of the core growth calculation and physical assumptions, see Hubickyj et al. 2005).”
THE ROLE OF MULTIPLICITY IN DISK EVOLUTION AND PLANET FORMATION (2011, background): “…al. 2008) either is not set by disk dissipation shutting off giant planet formation, or is evidence that the disk dissipation timescale is very well- matched to the giant planet formation timescale (∼3 Myr for core accretion; Pollack et al. 1996; Hubickyj et al. 2005; Dodson-Robinson et al. 2008).”
The effect of gas drag on the growth of protoplanets. Analytical expressions for the accretion of small bodies in laminar disks (2010, background): “Although the core accretion model (Pollack et al. 1996; Hubickyj et al. 2005) in its initial stages, i.e., before the formation of a ∼10 Earth mass (M⊕) core, concerns the accumulation of solid bodies, the role of the gas cannot be overstated.”
UNVEILING THE STRUCTURE OF PRE-TRANSITIONAL DISKS (2010, background): “It is feasible to form planets within 1 Myr, the age of our pre-transitional disk sample, via the two leading theories of planet formation: the gas instability model and the core nucleated accretion model.”
A dual-frequency sub-arcsecond study of proto-planetary disks at mm wavelengths: first evidence for radial variations of the dust properties (2011, background): “Competing models are the coreaccretion mechanism (e.g. Hubickyj et al. 2005), which faces apparent timescale difficulties, and the gravitational instability (e.g. Boss 1997; Rice et al. 2005), which requires massive disks.”
THE EFFECTS OF SNOWLINES ON C/O IN PLANETARY ATMOSPHERES (2011, background): “When sufficiently massive, the core accretes a gaseous envelope (Pollack et al. 1996; Hubickyj et al. 2005).”
Extrasolar planet population synthesis I: Method, formation tracks and mass-distance distribution (2009, methodology): “Therefore, each formation model applied to discuss extrasolar planet formation should also be put to the test to reproduce the characteristics of our own giant planets (Pollack et al. 1996, Alibert et al. 2005b; Hubickyj et al. 2005; Benvenuto & Brunini 2005).”
Models of Jupiter's growth incorporating thermal and hydrodynamic constraints (2008, background): “…(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, hereafter HBL05; Alibert et al. 2005a,b; Marley et al. 2007) or the disk interaction physics that governs the flow of gas to a…”
The Interior Structure, Composition, and Evolution of Giant Planets (2009, background): “…state” Marley et al. (2007) examined the issue of the accuracy of the arbitrary initial conditions (termed a “hot start” by the authors) by using initial conditions for cooling that were not arbitrary, but rather were given by a leading core accretion planet formation model (Hubickyj et al. 2005).”
The primordial nucleus of comet 67P/Churyumov-Gerasimenko (2015, background): “Studies of giant planet formation (e.g., Pollack et al. 1996; Alibert et al. 2005; Hubickyj et al. 2005; Dodson-Robinson et al. 2008; Weidenschilling 2008) and migration (e.g., Masset & Snellgrove 2001; Morbidelli & Crida 2007; Morbidelli et al. 2007; Walsh et al. 2011) in a gas disk show that…”
Mapping the Shores of the Brown Dwarf Desert. I. Upper Scorpius (2007, background): “Core accretion requires several Myr to form giant planets from protoplanetary disks (Hubickyj et al. 2005), while disk instability is most efficient at much younger ages (.0.5 Myr, Boss 2001).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, neutral): “…on the canonical “core accretion” scenario, a scaled-up MMSN disk can produce giant planets on timescales of ∼3-8 Myr (Pollack et al. 1996; Inaba et al. 2003; Hubickyj et al. 2005; Lissauer & Stevenson 2007), roughly consistent with the upper bound on disk lifetimes (e.g., Haisch et al. 2001).”
Dead Zone Accretion Flows in Protostellar Disks (2008, background): “The rapid sunward migration of the cores of Jupiter and Saturn is a difficulty for the standard model of giant planet formation by core accretion (Hubickyj et al. 2005).”
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…”
A Submillimeter View of Circumstellar Dust Disks in ρ Ophiuchi (2007, result): “…are indeed common, the giant planet formation process may be rapidly accelerated via direct condensations from spiral density waves/rings (e.g., Boss 1998; Mayer et al. 2007), compared to the standard core accretion and gas capture models (e.g., Pollack et al. 1996; Hubickyj et al. 2005).”
Formation of Giant Planets (2004, background): “…structure of a convective-radiative envelope is Mc = ( 2 3 )( 3 4 ) M = 1 2 M. (5) This is the often-quoted result that rapid envelope growth by gas accretion begins after the cross-over mass is achieved, that is when Me =Mc (e.g., Pollack et al. 1996; Hubickyj et al. 2005; Lissauer et al. 2009).”