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Formation of the Giant Planets

Published online by Cambridge University Press:  14 August 2015

Hiroshi Mizuno
Hiroshi Mizuno*
Affiliation:
Department of Physics, Kyoto University, Kyoto 606, Japan

Extract

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The structure of a gaseous envelope surrounding a icy/rocky core is studied in consideration of radiative transfer. It is found that when the core grows beyond a critical core mass, the envelope cannot be in equilibrium and collapses onto the core to form a proto-giant planet. The results are as follows (for details, see Mizuno 1980).

1) The critical core mass is smaller than that estimated by Perri and Cameron (1974) and Mizuno, Nakazawa and Hayashi (1978). 2) When the grain opacity in the envelope varies from 0 to 1 cm2/g, the critical core mass changes from ~2 to ~12 Earth's masses. 3) The critical core mass is independent of the region in the solar nebula.

These are due to the existence of the radiative region in the envelope.

Type
Session 3: Origin of the Solar System
Information
Symposium - International Astronomical Union , Volume 93: Fundamental Problems in the Theory of Stellar Evolution , 1981 , pp. 133 - 134
Copyright
Copyright © Reidel 1981 

References

Mizuno, H. 1980, Prog. Theor. Phys. 64, No.2, in press.CrossRefGoogle Scholar
Perri, F. and Cameron, A.G.W. 1974, Icarus 22, 416.CrossRefGoogle Scholar
Mizuno, H., Nakazawa, K. and Hayashi, C. 1978, Prog. Theor. Phys. 60, 699.CrossRefGoogle Scholar
Slattery, W.L. 1977, Icarus 32, 58.CrossRefGoogle Scholar
Hubbard, W.B. and MacFarlane, J.J. 1980, J. Geophys. Res. 85, 225.CrossRefGoogle Scholar