Models of the formation of the planets in the 47 UMa system

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, assumed to be high-temperature silicates, are in the dust form, to the stage when most solids are locked in planetesimals. The simulation of planetary evolution starts with a solid embryo of ~1 Earth mass, and proceeds according to the core accretion -- gas capture model. Orbital parameters are kept constant, and it is assumed that the environment of each planet is not perturbed by the second planet. 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 $\alpha \approx 0.01$. 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 \~3 Myr, while a planet of 0.89 Jupiter masses (the minimum for the outer planet) 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 167 and an initial radius of 40 AU.

Accepted for publication in A&A. 10 pages, 10 figures

References in corpus (4)

• Disk Frequencies and Lifetimes in Young Clusters
• Models of the in situ formation of detected extrasolar giant planets
• Nested-grid calculations of disk-planet interaction
• Rapid Formation of Ice Giant Planets

Cited by in corpus (11)

• Core-Accretion Model Predicts Few Jovian-Mass Planets Orbiting Red Dwarfs
• Models of Chemistry, Thermal Balance and Infrared Spectra from Intermediate-Aged Disks around G and K stars
• Giant Planet Migration through the Action of Disk Torques and Planet Scattering
• Migration of planets embedded in a circumstellar disk
• Formation of giant planets in disks with different metallicities
• Formation and Evolution of Planetary Systems: Upper Limits the Gas Mass in HD105
• Formation of giant planets around stars with various masses
• An alternative look at the snowline in protoplanetary disks
• Upper limits on CO 4.7 micron emission from disks around five Herbig Ae/Be stars
• Radial Distribution of Planets. Predictions based on the Core Accretion Gas Capture Planet formation Model
• Exocomets in the 47 UMa System: Theoretical Simulations including Water Transport