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Three-Dimensional Interaction between a Planet and an Isothermal Gaseous Disk. I. Corotation and Lindblad Torques and Planet Migration
Gravitational interaction between a planet and a three-dimensional isothermal gaseous disk is studied. In the present paper we mainly examine the torque on a planet and the resultant radial migrationExpand
Protoplanet Migration by Nebula Tides
Abstract The tidal interaction of a protoplanet with a circumstellar gaseous disk results in mutual angular momentum exchange that modifies both the disk and the orbit of the secondary. There areExpand
Formation of the Galilean Satellites: Conditions of Accretion
We examine formation conditions for the Galilean satellites in the context of models of late-stage giant planet accretion and satellite-disk interactions. We first reevaluate the current standard, inExpand
Three-dimensional Interaction between a Planet and an Isothermal Gaseous Disk. II. Eccentricity Waves and Bending Waves
We perform linear calculations to investigate three-dimensional density waves excited by planets on elliptical and inclined orbits in isothermal protoplanetary disks. We consider small planets thatExpand
A common mass scaling for satellite systems of gaseous planets
TLDR
It is shown that the overall properties of the satellite systems of Jupiter, Saturn and Uranus arise naturally, and it is suggested that similar processes could limit the largest moons of extrasolar Jupiter-mass planets to Moon-to-Mars size. Expand
The formation of planetesimals.
Four stages in the accretion of planetesimals are described. The initial stage is the condensation of dust particles from the gaseous solar nebula as it cools. These dust particles settle into a thinExpand
Survival of Planetary Systems
Gravitational interactions (i.e., disk tides) between a newly formed protoplanet and its precursor disk give rise to a net torque that drains angular momentum from the protoplanet's orbit. As aExpand
Tilting Saturn. I. Analytic Model
The tilt of Saturn's spin axis to its orbit plane is 267, while that of Jupiter is only 31. We offer an explanation for this puzzling difference owing to gravitational perturbations of Saturn by theExpand
Climatic variations on Mars: 1. Astronomical theory of insolation
This paper describes variations in the solar insolation on Mars that result from oscillations of the orbital eccentricity (0.005 ≲ e ≲ 0.141) and the obliquity (14.9° ≲ θ ≲ 35.5°) of the planet.Expand
Density waves in the solar nebula: Diffential Lindblad torque
Abstract The differential torque between a two-dimensional fluid disc and an embedded perturber due to waves launched at its resonances is calculated. For a non-self-gravitating disc, the disturbanceExpand
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