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Formation of the Giant Planets by Concurrent Accretion of Solids and Gas
New numerical simulations of the formation of the giant of the second phase. planets are presented, in which for the first time both the gas and The actual rates at which the giant planets accreted
On the Luminosity of Young Jupiters
Traditional thermal evolution models of giant planets employ arbitrary initial conditions selected more for computational expediency than physical accuracy. Since the initial conditions are
Models of the in Situ Formation of Detected Extrasolar Giant Planets
Abstract We present numerical simulations of the formation of the planetary companions to 47 UMa, ρ CrB, and 51 Peg. They are assumed to have formed in situ according to the basic model that a core
The role of turbulent convection in the primitive solar nebula. I - Theory. II - Results
A model of convective turbulence which takes radiative dissipation, rotation, and convective motion anisotropy into account, on the basis of a closure for the nonlinear interactions that employs the
Young jupiters are faint: new models of the early evolution of giant planets
Here we show preliminary calculations of the cooling and contraction of a 2 MJ planet. These calculations, which are being extended to 1–10 MJ, differ from other published “cooling tracks” in that
The role of turbulent convection in the primitive solar nebula II: Results
Abstract Numerical results from a new model of the primordial solar nebula are presented in which convection is assumed to be the sole source of turbulence that causes the nebula to evolve. We
A formula for the Shakura-Sunyaev turbulent viscosity parameter. [for modeling of accretion disks
A formula for the Shakura-Suniaev alpha parameter is proposed in terms of the growth rate of the unstable modes of the physical mechanisms that generates turbulence. Turbulent convection is discussed
Direct Numerical Simulations of Turbulent Convection
Turbulent convection may have played a major role in determining the structure and evolution of the primordial solar nebula, but current, incomplete models of convection and turbulence give very