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Formation of the Y Feature at the Venusian Cloud Top by Planetary‐Scale Waves and the Mean Circulation: Analysis of Venus Express VMC Images
Author(s) -
Nara Y.,
Imamura T.,
Murakami S.,
Kouyama T.,
Ogohara K.,
Yamada M.,
Takagi M.,
Kashimura H.,
Sato N.
Publication year - 2019
Publication title -
journal of geophysical research: planets
Language(s) - English
Resource type - Journals
eISSN - 2169-9100
pISSN - 2169-9097
DOI - 10.1029/2018je005779
Subject(s) - venus , rossby wave , zonal flow (plasma) , kelvin wave , zonal and meridional , geology , atmosphere of venus , geophysics , atmospheric circulation , atmospheric sciences , physics , climatology , astrobiology , plasma , quantum mechanics , tokamak
The relationship between the planetary‐scale ultraviolet contrast known as the Y feature and the wind field at the Venusian cloud top was investigated by using images obtained by Venus Monitoring Camera (VMC) on ESA's Venus Express. Spectral analyses of the ultraviolet reflectivity and the wind field revealed common periodicities of 4–5 Earth days, which are attributed to Kelvin and Rossby waves with a zonal wave number of unity. Combined with the morphological relationship between the dark streaks and the enhancement of poleward flow, we propose a mechanism for the formation of the Y feature: The dark materials are supplied to the cloud top in the equatorial region by a Kelvin wave, subsequently advected poleward by the mean meridional circulation and a Rossby wave, and then stretched by the midlatitude jet to the tilted band structures. A simplified transport model was developed to demonstrate the scenario.