Computer Science
Scientific paper
Mar 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996lpi....27..141b&link_type=abstract
Lunar and Planetary Science, volume 27, page 141
Computer Science
2
Jupiter, Nebulae: Solar, Planets: Formation
Scientific paper
Radiative hydrodynamical calculations of the thermal structure of an axisymmetric (2D) protoplanetary disk with a mass of 0.14 solar mass predict that the outer disk may be cool enough to become gravitationally unstable. The dynamical evolution of a 0.14 solar mass disk has been computed with a 3D hydrodynamics code in order to learn the outcome of gravitational instability in an intermediate-mass disk orbiting a solar-mass star. Growth of nonaxisymmetry occurs within a few rotation periods of the outer disk [P(sub)o], and the nonaxisymmetry is large enough to result in disk evolution through gravitational torques within about 100,000 yrs. After about 10 P(sub)o, the dominant m = 2 (bar) mode begins to saturate at an amplitude greater than 1--by this time, two Jupiter-mass clumps of gas have formed around 8 AU and continue to gain mass. The hot inner disk remains nearly axisymmetric throughout this interval. The model suggests a "best of both worlds" scenario may be tenable: formation of terrestrial planets through collisional accumulation in the hot inner nebula, and rapid formation of giant gaseous protoplanets in the cool outer nebula through gravitational instability of the disk.
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