期刊
ICARUS
卷 181, 期 2, 页码 458-464出版社
ACADEMIC PRESS INC ELSEVIER SCIENCE
DOI: 10.1016/j.icarus.2005.12.004
关键词
Jupiter, interior; extrasolar planets
Zonal winds simulated in two-dimensional computer models of turbulent convection in the equatorial plane of giant planets have greater Surface amplitudes for cases with smaller solid cores, and therefore larger buoyancy driving, all other properties being equal. This differential rotation in radius is maintained by the convergence of angular momentum flux, which occurs because of the convective flow that develops due to the effects of planetary rotation and density stratification. The superposition of the convective flow and the stronger zonal flow produces wave-like. instead of cellular convection. (c) 2005 Elsevier Inc. All rights reserved.
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