Giant planet formation
- G. Wuchterl
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The accumulation of giant planets involves processes typical for terrestrial planet formation as well as gasdynamic processes that were previously known only in stars. The condensible element cores of the gas-giants grow by solid body accretion while envelope formation is governed by ‘stellar-like’ equilibria and the dynamic departures thereof. Two hypotheses for forming Uranus/Neptune-type planets — at sufficiently large heliocentric distances while allowing accretion of massive gaseous envelopes, i.e. Jupiter-type planets at intermediate distances — have been worked out in detailed numerical calculations: (1) Hydrostatic gas-accretion models with time-dependent solid body accretion-rates show a slow-down of core-accretion at the appropriate masses of Uranus and Neptune. As a consequence, gas-accretion also stagnates and a window is opened for removing the solar nebula during a time of roughly constant envelope mass. (2) Gasdynamic calculations of envelope accretion for constant planetesimal accretion-rates show a dynamic transition to new envelope equilibria at the so called critical mass. For a wide range of solar nebula conditions the new envelopes have respective masses similar to those of Uranus and Neptune and are more tightly bound to the cores. The transitions occur under lower density conditions typical for the outer parts of the solar nebula, whereas for higher densities, i.e. closer to the Sun, gasdynamic envelope accretion sets in and is able to proceed to Jupiter-masses.
- Bodenheimer, P. and Pollack, J.B. (1986) Calculations of the accretion and evolution of the giant planets: The effect of solid cores,Icarus 67, 391–408.
- Boss, A.P., Morfill, G.E., and Tscharnuter, W.M. (1989) Models of the Formation and Evolution of the Solar Nebula, in S.K. Atreya, J.B. Pollack and M.S. Matthews, (eds.),Origin and Evolution of Planetary and Satellite Atmospheres, Univ. of Arizona Press, Tucson, pp. 35–77.
- Chabrier, G., Saumon, D., Hubbard, W.D., and Lunine, J.I. (1992) The Molecular-Metallic Transition of Hydrogen and the Structure of Jupiter and Saturn,Astrophys. Journ. 319, 817–826.
- Greenzweig, Y. and Lissauer, J.J. (1990) Accretion Rates of Protoplanets II. Gaussian Distribution of Planetesimal Velocities,Icarus 100, 440–463.
- Götz, M. (1993)Die Entwicklung yon Proto-Gasplaneten mit Drehimpuls — Strahlungshydrodynamische Rechnungen, Dissertation, Univ. Heidelberg.
- Hubbard, W.B. and Marley, M.S. (1989) Optimized Jupiter, Saturn and Uranus Interior Models,Icarus 78, 102–118.
- Hubbard, W.B., Nellis, W.J., Mitchell, A.C., Holmes, N.C., Limaye, S.S., and McCandless, P.C. (1991) Interior Structure of Neptune: Comparison with Uranus,Science 253, 648–651.
- Kippenhahn, R. and Weigert, A. (1990)Stellar Structure and Evolution, Springer-Verlag, Berlin.
- Korycansky, D.G., Bodenheimer, P., and Pollack, J.B. (1991) Numerical models of giant planet formation with rotation,Icarus 92, 234–251.
- Kusaka, T., Nakano, T. and Hayashi, C. (1970) Growth of Solid Particles in the Primordial Solar Nebula,Prog. Theor. Phys. 44, 1580–1595.
- Lissauer, J.J., Pollack, J.B., Wetherill, G.W. and Stevenson, D.J., (1995) Formation of the Neptune System, inNeptune Univ. Arizona Press, in prep.
- Mizuno, H. (1980) Formation of the Giant Planets,Prog. Theor. Phys. 64, 544–557.
- Perri, F. and Cameron, A.G.W. (1974) Hydrodynamic instability of the solar nebula in the presence of a planetary core,Icarus 22, 416–425.
- Pollack, J.B. (1985) Formation of the giant planets and their satellite-ring systems: An overview, in D.C. Black and M.S. Matthews (eds.)Protostars and Planets II, Univ. Arizona Press, Tucson.
- Stevenson, D.J. (1982) Formation of the giant planets,Planet. Space Sci. 30, 755–764.
- Stevenson, D.J. (1984) On forming giant planets quickly (superganymedean puffballs!),Lunar Planet. Sci. XV, 821–822 (abstract).
- Tajima, N. (1994)Giant Planet Formation: Dynamical Stability of the Envelope, Master Thesis, Univ. Tokyo.
- Wuchterl, G. (1990) Hydrodynamics of Giant Planet Formation I: Overviewing theκ-MechanismAstron. Astrophys.,238:83–94.
- Wuchterl, G. (1991a) Hydrodynamics of Giant Planet Formation II: Model Equations and Critical MassIcarus 91, 39–52.
- Wuchterl, G. (1991b) Hydrodynamics of Giant Planet Formation III: Jupiter's Nucleated Instability” ’.Icarus 91, 53–64.
- Wuchterl, G., 1993 The Critical Mass for Protoplanets Revisited: Massive Envelopes Through Convection” ’.Icarus 106, 323–334.
- Zharkov, V.N. and Gudkova, T.V. (1991)Ann. Geophys. 9, 357.
- Zharkov, V.N. and Gudkova, T.V. (1992) Modern Models of Giant Planets, in Y. Soyono and M.H. Manghnani (eds.),High Pressure Research: Application to Earth and Planetary Sciences, Terra Sci. Publ. Co. (TERRAPUB), Tokyo / American Geophysical Union, Washington, D.C..
- Giant planet formation
Earth, Moon, and Planets
Volume 67, Issue 1-3 , pp 51-65
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- Kluwer Academic Publishers
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- G. Wuchterl (1)
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- 1. Institut für Astronomie der Universität Wien, Türkenschanzstraß 17, A-1180, Wien, Austria