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| Paper: |
Formation of the 47 UMa System |
| Volume: |
294, Scientific Frontiers in Research on Extrasolar Planets |
| Page: |
311 |
| Authors: |
Bodenheimer, P.; Kornet, K.; Różyczka, M. |
| Abstract: |
Formation of planets in the 47 UMa system is followed in an evolving protoplanetary disk composed of gas and solids. The evolution of the disk is calculated from an early stage, when all solids are in the dust form, to the stage when most solids are locked in planetesimals. The simulation of planetary evolution starts when the planetesimals have formed a solid embryo of about 1 Earth mass, and proceeds according to the core accretion -- gas capture model. It is found that conditions suitable for both planets to form within several Myr are easily created, and maintained throughout the formation time, in disks with α≈0.01. In such disks, a planet of 2.6 Jupiter masses (the minimum for the inner planet of the 47 UMa system) may be formed at 2.1 AU from the star in about 3 Myr, while a planet of 0.89 Jupiter masses (the minimum for the outer planet of the 47 UMa system) may be formed at 3.95 AU from the star in about the same time. The formation of planets is possible as a result of a significant enhancement of the surface density of solids between 1.0 and 4.0 AU, which results from the evolution of a disk with an initially uniform gas-to-dust ratio of 100 and an initial radius of 40 AU. |
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