The orbital evolution of planets in disks
نویسنده
چکیده
The orbital parameters of the observed extrasolar planets differ strongly from those of our own solar system. The differences include planets with high masses, small semi-major axis and large eccentricities. We performed numerical computations of embedded planets in disks and follow their mass growth and orbital evolution over several thousand periods. We find that planets do migrate inwards on timescales of about 10 years on nearly circular orbits, during which they may grow up to about 5 Jupiter masses. The interaction of the disk with several planets may halt the migration process and lead to a system similar to the solar planetary system.
منابع مشابه
Planet-planet Scattering in Planetesimal Disks
We study the final architecture of planetary systems that evolve under the combined effects of planet-planet and planetesimal scattering. Using N-body simulations we investigate the dynamics of marginally unstable systems of gas and ice giants both in isolation and when the planets form interior to a planetesimal belt. The unstable isolated systems evolve under planet-planet scattering to yield...
متن کاملOrbital Evolution and Migration of Giant Planets: Modeling Extrasolar Planets
Giant planets in circumstellar disks can migrate inward from their initial (formation) positions. Radial migration is caused by inward torques between the planet and the disk; by outward torques between the planet and the spinning star; and by outward torques due to Roche lobe overflow and consequent mass loss from the planet. We present self-consistent numerical considerations of the problem o...
متن کاملHalting Planet Migration in the Evacuated Centers of Protoplanetary Disks
Precise Doppler searches for extrasolar planets find a surfeit of planets with orbital periods of 3–4 days, and no planets with orbital periods less than 3 days. The circumstellar distance, R0, where small grains in a protoplanetary disk reach sublimation temperature (∼ 1500 K) corresponds to a period of∼ 6 days. Interior to R0, turbulent accretion due to magneto-rotational instability may evac...
متن کاملGravitational instability in binary protoplanetary disks; new constraints on giant planet formation
We use high resolution 3D SPH simulations to study the evolution of selfgravitating binary protoplanetary disks. Heating by shocks and cooling are included. We consider different orbital separations and masses of the disks and central stars. Isolated massive disks (M ∼ 0.1M⊙) fragment into protoplanets as a result of gravitational instability for cooling times comparable to the orbital time. Fr...
متن کاملImaging Protoplanetary Disks with a Square Kilometer Array
The recent detections of extrasolar giant planets has revealed a surprising diversity of planetary system architectures, with many very unlike our Solar System. Understanding the origin of this diversity requires multiwavelength studies of the structure and evolution of the protoplanetary disks that surround young stars. Radio astronomy and the Square Kilometer Array will play a unique role in ...
متن کامل