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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 accretedExpand
Orbital migration of the planetary companion of 51 Pegasi to its present location
THE recent discovery1 and confirmation2 of a possible planetary companion orbiting the solar-type star 51 Pegasi represent a breakthrough in the search for extrasolar planetary systems. Analysis ofExpand
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 areExpand
The N2K Consortium. II. A Transiting Hot Saturn around HD 149026 with a Large Dense Core
Doppler measurements from Subaru and Keck have revealed radial velocity variations in the V = 8.15, G0 IV star HD 149026 consistent with a Saturn-mass planet in a 2.8766 day orbit. PhotometricExpand
Studies in Stellar Evolution. III. The Calculation of Model Envelopes.
The formal theory underlying existing techniques for representing the superadiabatic layers in convective envelopes is re-examined. Particular emphasis is placed on the discussion of points ofExpand
On the Radii of Extrasolar Giant Planets
We have computed evolutionary models for extrasolar planets that range in mass from 0.1MJ to 3.0MJ and that range in equilibrium temperature from 113 to 2000 K. We present four sequences of models,Expand
Accretion of the gaseous envelope of Jupiter around a 5–10 Earth-mass core
Abstract New numerical simulations of the formation and evolution of Jupiter are presented. The formation model assumes that first a solid core of several M ⊕ accretes from the planetesimals in theExpand
On the Tidal Inflation of Short-Period Extrasolar Planets*
We examine the consequences of tidal interaction between eccentric short-period extrasolar planets and their host stars and of secular perturbations between planets in a given system. If the planetExpand
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 coreExpand
Calculations of the accretion and evolution of giant planets: The effects of solid cores
The evolution of the giant planets is calculated under the general hypothesis that the solid cores formed first, by accretion of small particles, and that these cores later gravitationally attractedExpand
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