Forming Planetary Cores in a Turbulent Non-Isothermal Disk

Details Forming Planetary Cores in a Turbulent Non-Isothermal Disk Forming Planetary Cores in a Turbulent Non-Isothermal Disk

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf.1522h&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.1522

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Scientific paper

Non-Isothermal disks have been shown to have regions where the net torque on a planet is positive, leading to outward migration of the planet. When a region with negative torque is directly exterior to this, planets in the inner region migrate outwards and planets in the outer region migrate inwards, converging where the torque is zero. We incorporate the torques from an evolving non-isothermal disk into an N-body simulation, and find that the bodies do converge to the zero torque region, but effects of neighbouring planets prevents the planets from merging. Though N-body interactions prevent complete merging to form one core, the addition of a weak stochastic force to simulate turbulence in the disk allows for orbit crossings and mergers near the convergence zone. In this way, it is possible to move from the sub-Earth mass regime into the 10 Earth mass planetary core regime in 2-3 million years.

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