Zonal winds near Venus' cloud top level: An analytic model of the equatorial wind speed |
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| Institution: | 1. CETESB—Companhia Ambiental de São Paulo, Av. Prof. Frederico Hermann Jr., 345, CEP 05459-900 São Paulo, SP, Brazil;2. Instituto de Botânica, CP 3005, CEP 01031-970 São Paulo, SP, Brazil;3. Universidade de São Paulo, Instituto de Biociências, CP 11461, CEP 05422-970 São Paulo, SP, Brazil;1. A.F. Ioffe Physico-Technical Institute, St. Petersburg, Russia;2. Metla, Rovaniemi Research Unit, PO Box 16, FI 96301 Rovaniemi, Finland;3. Central Astronomical Observatory at Pulkovo, Russia;4. St. Petersburg State University, St. Petersburg, Russia;1. Department of Chemistry, Smith College, Northampton, MA 01063, USA;2. Chemistry Department, Trinity Washington University, Washington, DC 20017, USA;1. Electrical Engineering Department, Guangxi University, Nanning 530004, China;2. Shantou Power System Group Corporation, Shantou 515000, Guangdong, China |
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| Abstract: | It is proposed that the equatorial wind speed near Venus' cloud top level is maintained by a balance between the pumping effect of the semidiurnal tide and vertical advection by the Hadley circulation, both integrated across the thermal driving region. A consequence of this hypothesis is that the maximum equatorial zonal wind speed is proportional to Nh where N is buoyancy frequency and h is a measure of the thickness of the driving region. The proportionality constant is a weakly increasing function of the heating rate and a decreasing function of λh, where λ is an inverse length characterizing the mean zonal wind shear. The equilibrium solution considered is shown to be stable. For the class of solutions investigated, there is a threshold value of heating rate below which there is no equilibrium satisfying the hypothesized balance, but this result depends on the assumption that the shape of the zonal wind profile is invariant with thermal forcing amplitude. |
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