Calculations of the early evolution of Jupiter

Abstract The evolution of the protoplanet Jupiter is followed, using a hydrodynamic computer code with radiative energy transport. Jupiter is assumed to have formed as a subcondensation in the primitive solar nebula at a density just high enough for gravitational collapse to occur. The initial state has a density of 1.5 × 10 −11 g cm −3 and a temperature of 43 K; the calculations are carried to an equilibrium state where the central density reaches 0.5 g cm −3 and the central temperature reaches 2.5 × 10 4 K. During the early part of the evolution the object contracts in quasi-hydrostatic equilibrium; later on hydrodynamic collapse occurs, induced by the dissociation of hydrogen molecules. After dissociation is complete, the planet regains hydrostatic equilibrium with a radius of a few times the present value. Further evolution beyond this point is not treated here; however the results are consistent with the existence of a high-luminosity phase shortly after the planet settles into its final quasistatic contraction.

[1]  J. Pollack,et al.  The structure and evolution of Jupiter - The fluid contraction stage , 1975 .

[2]  A. Cameron,et al.  Accumulation processes in the primitive solar nebula , 1973 .

[3]  H. Aumann,et al.  The internal powers and effective temperatures of Jupiter and Saturn. , 1969 .

[4]  P. Bodenheimer,et al.  DYNAMIC COLLAPSE OF THE ISOTHERMAL SPHERE. , 1968 .

[5]  J. N. Stewart,et al.  RADIATIVE AND CONDUCTIVE OPACITIES FOR ELEVEN ASTROPHYSICAL MIXTURES , 1965 .

[6]  J. Auman.  The infrared opacity of hot water vapor , 1968 .

[7]  L. G. Henyey,et al.  A NEW METHOD OF AUTOMATIC COMPUTATION OF STELLAR EVOLUTION , 1964 .

[8]  C. Hayashi,et al.  Rapid Contraction of Protostars to the Stage of Quasi-Hydrostatic Equilibrium. III Stars of 0.05, 1.0 and 20M⊙ with Energy Flow by Radiation and Convection , 1970 .

[9]  P. Bodenheimer.  The Evolution of Protostars of 1 and 12 Solar Masses , 1968 .

[10]  James B. Pollack,et al.  Implications of Jupiter's Early Contraction History for the Composition of the Galilean Satellites , 1974 .

[11]  J. N. Stewart,et al.  ROSSELAND OPACITY TABLES FOR POPULATION I COMPOSITIONS. , 1970 .

[12]  A. Cameron,et al.  Models of the Giant Planets , 1974 .

[13]  R. Smoluchowski,et al.  Structure of Jupiter and Saturn , 1973 .

[14]  W. Hubbard.  Structure of Jupiter - Chemical composition, contraction, and rotation , 1970 .

[15]  A. Cameron,et al.  Numerical models of the primitive solar nebula. , 1973 .

[16]  D. Haar,et al.  Historical Review of Theories of the Origin of the Solar System , 1963 .

[17]  J. Pollack,et al.  An evolutionary calculation of Jupiter. , 1972 .

[18]  F. Low.  Observations of Venus, Jupiter, and Saturn at λ20 μ. , 1966 .

[19]  J. Gaustad.  THE OPACITY OF DIFFUSE COSMIC MATTER AND THE EARLY STAGES OF STAR FORMATION , 1963 .

[20]  J. Gaustad,et al.  ROSSELAND AND PLANCK MEAN ABSORPTION COEFFICIENTS FOR PARTICLES OF ICE, GRAPHITE, AND SILICON DIOXIDE. , 1969 .

[21]  T. Tsuji.  The atmospheric structure of late-type stars-1-Physical properties of cool gaseous mixtures and the effect of molecular line absorption on stellar opacities , 1966 .

[22]  D. Keeley.  The Static Structure of Long-Period Variable Stars , 1970 .

[23]  Richard B. Larson,et al.  Numerical Calculations of the Dynamics of a Collapsing Proto-Star , 1969 .

[24]  William B. Hubbard,et al.  Thermal Models of Jupiter and Saturn , 1969 .

[25]  R. Smoluchowski.  The interior structure of Jupiter: Consequences of Pioneer 10 data , 1975 .