Wind Measurements In Venus' Upper Mesosphere With The IRAM-Plateau De Bure Interferometer

Details Wind Measurements In Venus' Upper Mesosphere With The IRAM-Plateau De Bure Interferometer Wind Measurements In Venus' Upper Mesosphere With The IRAM-Plateau De Bure Interferometer

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.1504m&link_type=abstract

American Astronomical Society, DPS meeting #42, #15.04; Bulletin of the American Astronomical Society, Vol. 42, p.974

Computer Science

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Scientific paper

Venus' upper mesosphere (90-105 km altitude) is a region of dynamic transition between the troposphere, exhibiting retrograde zonal flow, and the thermosphere, driven by a subsolar-antisolar flow (SSAS). One possible method to measure the velocity field in the upper mesosphere is to map the Doppler-shift in the core of atmospheric lines in the mm/sub-mm range. Past observations of CO lines have revealed dynamic patterns most often interpreted as a combination of a SSAS flow and a retrograde zonal flow, with strong temporal variations (Clancy et al., 2006).
We present observations of the CO(1-0) line at 115 GHz obtained at the IRAM-Plateau de Bure Interferometer, on June 12 and 13, 2009. The spatial resolution achieved by the array (4-5") allowed a fine mapping of the line over Venus' disk (22"). The velocity fields obtained on both days display similar patterns, and are at odds with most previous observations.
On the day-hemisphere, the approaching wind observed is interpreted as a prograde zonal flow with an average velocity near the sub-solar point of 85 m/s. On the night-hemisphere, at mid-high latitudes, the recessing wind observed could be identified again with a prograde zonal flow, with an average wind velocity of 60 m/s in the Southern hemisphere, and of 110 m/s in the Northern hemisphere. Near the equator, a retrograde zonal wind is detected with velocities about 25 +/-8 m/s near the anti-solar point. The detection of a prograde zonal wind, with similar values as those reported here, was so far only claimed once by Lellouch et al. (2007).
A full physical analysis of the CO lines profiles will be presented. The estimations of the sounded level in the atmosphere will be used to provide an accurate interpretation of the observed velocity field, to be compared to the latest dynamical models and observations.

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