Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980mnras.191...37l&link_type=abstract
Monthly Notices of the Royal Astronomical Society, vol. 191, Apr. 1980, p. 37-48.
Astronomy and Astrophysics
Astronomy
220
Astronomical Models, Interplanetary Medium, Protoplanets, Stellar Mass Accretion, Sun, Convection, Planetary Evolution, Planetary Mass, Solar System
Scientific paper
A self-consistent accretion disk model is proposed for the primordial solar nebula. In this model convective motion not only transports energy in the z-direction but also provides a mechanism for viscous coupling in the disk so that energy stored in shear motion can be dissipated. It is found that a steady-state accretion disk model can be constructed. Conditions for the primordial solar nebula to contain the present planetary mass are obtained. The results presented here tend to favor the idea that the planets formed by the accumulation of planetesimals, rather than by gravitational instability, occurring on a scale comparable to their present mass. It is concluded that the tidal influence of a growing planet on the disk, coupled with the conditions required for formation, automatically gives rise to an upper limit of approximately 0.001 solar mass for a planet's mass.
Lin Doug N. C.
Papaloizou John
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