Inertia coefficient considerations and the structure of Jovian planets

Details Inertia coefficient considerations and the structure of Jovian planets Inertia coefficient considerations and the structure of Jovian planets

Sep 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983cemec..31...81d&link_type=abstract

Celestial Mechanics (ISSN 0008-8714), vol. 31, Sept. 1983, p. 81-94.

Astronomy and Astrophysics

Astronomy

3

Astronomical Models, Density (Mass/Volume), Gas Giant Planets, Inertia, Planetary Structure, Jupiter (Planet), Planetary Mass, Saturn (Planet), Planets, Giant Planets, Inertia, Structure, Comparisons, Jupiter, Saturn, Models, Density, Surface, Interior, Theoretical Studies

Scientific paper

It is noted that modern hydrostatic models of the Jovian planets use as observational constraints, in addition to the total mass and radius, the coefficients J2, J3, . . . of the external gravity potential. It is only the quadrupole moment, J2, however, that has been determined for Jupiter and Saturn to a high degree of accuracy, that is, to four significant figures. The hexadecapole moment, J4, does not seem to be known to an accuracy of any better than 10 percent. What is more, the exact rotation law is known for neither Jupiter or Saturn. For this reason, continuous two-parameter models based on mean density and inertial coefficient adjustments can still be defended on the grounds of simplicity, at least as starting models for computing more sophisticated models at a later stage. It is shown that for Jupiter, a density law of the form rho = rho0(1 - x to the n power) is adequate as a simplified representation that is consistent with current information. For Saturn, however, the law is not adequate.

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