Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.1127h&link_type=abstract
American Astronomical Society, DPS meeting #42, #11.27; Bulletin of the American Astronomical Society, Vol. 42, p.1022
Astronomy and Astrophysics
Astronomy
Scientific paper
The interior structures of Uranus and Neptune are not well constrained. We present 'empirical' models (pressure vs. density) of Uranus and Neptune interiors constrained by the gravitational coefficients J2, J4, and the planetary radii and masses, using Voyager's solid-body rotation periods. The empirical pressure-density profiles are then interpreted in terms of physical equations of state of hydrogen, helium, ice (H2O), and rock (SiO2) to test the physical plausibility of the models. The interiors of Uranus and Neptune are found to be very similar. Our analysis suggests that the concentration of heavier elements inside both Uranus and Neptune interiors could increase gradually towards the planetary centers, without having sharp compositional transitions as typically assumed.
Uranus and Neptune (solid-body) rotation periods, 17.24h and 16.11h, respectively, are based on Voyager 2 measurements of variations in the planets' radio signals and on fits to the planets' magnetic fields.
The realization that Saturn's radio period does not represent the planet's deep interior rotation and the complexity of the magnetic fields of Uranus and Neptune raise the possibility that the Voyager 2 radio and magnetic periods might not represent the deep interior rotation periods of the planets. We use wind and shape data to investigate the rotation of Uranus and Neptune. Minimization of wind velocities or dynamic heights of the 1 bar isosurfaces, constrained by the single occultation radii and gravitational coefficients of the planets, leads to solid-body rotation periods of 16.58h for Uranus and 17.46h for Neptune. We derive shapes for the planets based on these rotation rates. Wind velocities with respect to these rotation periods are essentially identical on Uranus and Neptune and wind speeds are slower than previously thought. Alternatively, if we interpret wind measurements in terms of differential rotation on cylinders there are essentially no residual atmospheric winds.
Anderson John D.
Helled Ravit
Podolak Morris
Schubert Gerald
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