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Additional resources for An Introduction to Planetary Atmospheres

Example text

In the case of a deformable fluid body, the equilibrium figure resulting from the action of these forces is an ellipsoid. Rapidly spinning planets can widen along the equatorial axis due to the centrifugal force. In the solar system fluid planets, tidal deformations can also be produced by close satellites, although their effect on the planet shape is negligible when compared with that produced by rotation. However, in the extrasolar giant planets of “hot” or “very hot” Jupiter types, the tidal effect raised by the star on the planet can be important when compared with the effect of rotation for two reasons.

For E < 0, the orbit is closed (bounded) and is an ellipse with extreme distances to the focus ra and rb. For the particular case ra = rb = r0 (corresponding to a minimum in the effective potential energy), the elliptic motion reduces to a simple circle. 13) where a is the semimajor axis of the ellipse e is the eccentricity (defined as the ratio of the distance between the two foci of the ellipse and the distance 2a) 10 An Introduction to Planetary Atmospheres For an ellipse, 0 < e < 1 (e = 0 for circular motion).

For the terrestrial planets and major satellites that are approximately spherical, the “J-coefficients” are small and can be neglected. However, the oblateness of the giant planets makes the J-coefficients substantial, giving important information on their internal structure and deep atmospheres. They are measured by observing the gravitational perturbations acting on satellites, rings, and spacecrafts in orbit around the planet or during a fly-by. As discussed in Chapter 7, a family of models for the atmospheric circulation in the giant planets proposes that motions extend deep in the atmosphere, occupying a significant fraction of the planetary radius.

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