Jupiter's Rotation Period Derived from Minimization of the Dynamic Heights of its Isobaric Surface

Details Jupiter's Rotation Period Derived from Minimization of the Dynamic Heights of its Isobaric Surface Jupiter's Rotation Period Derived from Minimization of the Dynamic Heights of its Isobaric Surface

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.5305h&link_type=abstract

American Astronomical Society, DPS meeting #40, #53.05; Bulletin of the American Astronomical Society, Vol. 40, p.494

Astronomy and Astrophysics

Astronomy

Scientific paper

Anderson & Schubert (2007, Science, 317,1384) proposed that Saturn's rotation period might be ascertained by minimizing the dynamic height of the 100 mbar isosurface with respect to the geoid; they derived a rotation period of 10h:32m:35s. We investigate the same approach for Jupiter to see if the Jovian rotation period is predicted by minimizing the dynamical heights of its isobaric surface. The shape of the Jovian pressure isosurface is derived from zonal wind data (García-Melendo & Sanchez-Lavega, 2001, Icarus, 316) and the Jovian geoid. Then, by regarding the Jovian geoid as undetermined in terms of Jupiter's rotation rate, we vary the rotation rate and the geoid and search for the geoid that minimizes the dynamical heights of the pressure isosurface in an rms sense.
A rotation period of 9h:54m:29.7s is found to minimize the dynamical heights of the pressure isosurface. This rotation period is only one minute shorter than the measured period of Jupiter. The successful application of the method to Jupiter lends support to its relevance for Saturn.

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