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The population of known extrasolar planets includes giant and terrestrialplanets that closely orbit their host star. Such planets experience significanttidal distortions that can force the planet into synchronous rotation. Thecombined effects of tidal deformation and centripetal acceleration inducessignificant asphericity in the shape of these planets, compared to the mildoblateness of Earth, with maximum gravitational acceleration at the poles. Herewe show that this latitudinal variation in gravitational acceleration isrelevant for modeling the climate of oblate planets including Jovian planetswithin the solar system, closely-orbiting hot Jupiters, and planets within thehabitable zone of white dwarfs. We compare first- and third-orderapproximations for gravitational acceleration on an oblate spheroid andcalculate the geostrophic wind that would result from this asphericity on arange of solar system planets and exoplanets. Third-order variations ingravitational acceleration are negligible for Earth but become significant forJupiter, Saturn, and Jovian exoplanets. This latitudinal variation ingravitational acceleration can be measured remotely, and the formalismpresented here can be implemented for use in general circulation climatemodeling studies of exoplanet atmospheres.

Geostrophic wind induced by latitudinal variation in gravitational acceleration on oblate planets