Leroy, Stephen S. and Ingersoll, Andrew P. (1995) Convective Generation of Gravity Waves in Venus's Atmosphere: Gravity Wave Spectrum and Momentum Transport. Journal of the Atmospheric Sciences, 52 (21). pp. 3717-3737. ISSN 0022-4928. http://resolver.caltech.edu/CaltechAUTHORS:LERjas95
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The emission of internal gravity waves from a layer of dry convection embedded within a stable atmosphere with static stability and zonal winds varying in height is calculated. This theory is applied to Venus to investigate whether these waves can help support the westward maximum of angular momentum of Venus's middle atmosphere. The emission mechanism is similar to that suggested for driving the gravity modes of the Sun and relates the amplitude and spectrum of the waves to the amplitude and spectrum of the convection. Waves are damped by several mechanisms: wavebreaking in the stable atmosphere, critical layer absorption, reabsorption by the convection, and wave radiation to space. The authors use plane parallel geometry without rotation and assume sinusoidal wave fluctuations in the horizontal dimensions. The vertical dependence is determined using the WKBJ approximation. It is found that convectively generated gravity waves do not exert an acceleration where the westward winds are greatest. Instead, they deposit westward momentum in a 1-km thick layer just above the convection. Other waves deposit eastward momentum far above the westward wind maximum where decelerations can exceed 20 m s^−1 day^−1, comparable to deceleration amplitudes in Earth's mesosphere. Although the momentum fluxes by gravity waves are substantial, the vertical profile of acceleration does not match what is required for supporting Venus's atmospheric superrotation.
|Additional Information:||© 1995 American Meteorological Society. (Manuscript received October 31, 1994, in final form April 7, 1995) We wish to thank Peter Goldreich for much assistance in this work. It was supported by a National Science Foundation Graduate Research Fellowship and by NAGW-1956 of the NASA Planetary Atmospheres program. Division of Geological and Planetary Sciences of the California Institute of Technology Contribution No. 5458.|
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