منابع مشابه
Oligarchic Growth of Protoplanets
and N-body calculations (e.g., Ida 1990, Ida and Makino 1992b). It is shown that dynamical friction is effective in We investigate the growth and the orbital evolution of proa Keplerian potential as well as in a free space. Kokubo toplanets embedded in a swarm of planetesimals using threedimensional N-body simulations. We find that among protoplaand Ida (1996), hereafter referred to as Paper I,...
متن کاملOutflows driven by Giant Protoplanets
We investigate outflows driven by a giant protoplanet using three-dimensional MHD nested grid simulations. We consider a local region around the protoplanet in the protoplanetary disk, and calculate three models: unmagnetized disk model, magnetized disk model having magnetic field azimuthally parallel to the disk, and magnetic field perpendicular to the disk. Outflows with velocities, at least,...
متن کاملHigher-Orders of Vagueness Reinstated
The role of higher-order vagueness in creating apparent difficulties with attempts to formulate a sentence capable of characterizing the vagueness of a predicate, that is, its role in appearing to undermine a characteristic-sentence approach to defining vagueness, has led some to question the very existence of such a phenomenon. Hyde () sought to put the existence of higher-order vagueness ...
متن کاملMigration of Protoplanets in Radiative Disks
Context. In isothermal disks the migration of protoplanets is directed inward. For small planetary masses the standard type I migration rates are so fast that this may result in an unrealistic loss of planets into the stars. Aims. We investigate the planet-disk interaction in non-isothermal disks and analyze the magnitude and direction of migration for an extended range of planet masses. Method...
متن کاملCore Formation in Giant Gaseous Protoplanets
Sedimentation rates of silicate grains in gas giant protoplanets formed by disk instability are calculated for protoplanetary masses between 1 MSaturn to 10 MJupiter. Giant protoplanets with masses of 5 MJupiter or larger are found to be too hot for grain sedimentation to form a silicate core. Smaller protoplanets are cold enough to allow grain settling and core formation. Grain sedimentation a...
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ژورنال
عنوان ژورنال: Eos, Transactions American Geophysical Union
سال: 2006
ISSN: 0096-3941
DOI: 10.1029/2006eo140003