Physics
Scientific paper
Oct 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf..640h&link_type=abstract
EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.640
Physics
Scientific paper
General circulation in the Venusian mesosphere (70 - 110 km) is an important factor for the upward propagation of atmospheric waves. We have investigated effects of the mesospheric wind on the upward propagation of the planetary-scale waves generated in the Venusian cloud deck (50 - 70 km) with a General Circulation Model (GCM). Our GCM covers the altitude region between 80 km and about 180 km. We have performed simulations assuming three different wind velocity distributions at the lower boundary (LB). In case 1, the zonal wind velocity at the LB is 0 m/s. In case 2 and 3, the rigid body rotation with the equatorial wind velocity of 40 m/s and 80 m/s is assumed, respectively. The pressure and temperature at the LB is referred from the empirical model of the Venusian atmosphere (VIRA model) [1]. We imposed the Kelvin wave with the phase speed of about 110 m/s, which was observed from previous observations [2], at the LB. Our simulations show the propagation of the Kelvin wave up to around 130 km in all cases. However, the maximum amplitude of the zonal wind velocity fluctuation is smaller with the faster westward wind at the LB. The decrease of the wind velocity fluctuations is interpreted as the result of the vertical group velocity change of the Kelvin wave which is caused by the decrease of the intrinsic phase speed.
Fujiwara Hideaki
Hoshino N.
Kasaba Yasumasa
Takagi Masahiro
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