A&A 396, 977-986 (2002)
DOI: 10.1051/0004-6361:20021401
Models of the formation of the planets in the 47 UMa system
K. Kornet1, P. Bodenheimer2 and M. Rózyczka11 Nicolaus Copernicus Astronomical Center , Bartycka 18 , Warsaw, 00-716, Poland
e-mail: kornet@camk.edu.pl; mnr@camk.edu.pl
2 UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz,CA 95064, USA
e-mail: peter@ucolick.org
(Received 26 July 2002 / Accepted 19 September 2002 )
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
. 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.
Key words: stars: planetary systems -- stars: planetary systems: formation
Offprint request: K. Kornet, kornet@camk.edu.pl
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