Computer Science
Scientific paper
Jul 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009hst..prop12433j&link_type=abstract
HST Proposal ID #12433. Cycle 18
Computer Science
Scientific paper
Currently, there is an unprecedented opportunity to observe the atmosphere of Venus. The Japanese Venus Climate Orbiter {VCO} mission, successfully launched on May 21, 2010, will be observing Venus simultaneously with Venus Express {VEx} Mission from December 2010 onward. A campaign for Earth-based observations coincident with the arrival of VCO at Venus is currently under-way. Fortuitously, the window for observing Venus with HST at a solar elongation greater than 45 degrees is December 25, 2010, thru January 28, 2011. Thus, we are applying to use HST/STIS during that time to observe Venus upper cloud deck {65-75 km} in the ultraviolet {200-600 nm} at high spectral {0.3-0.6 nm} and spatial {40-60 km/pixel} resolution using the G230LB {0.17-0.31 nm} and G430L {0.30-0.57 nm} gratings, with the 52x0.1 slit and the CCD detector. By observing Venus with the slit in its nominal 45 degree orientation, we will map, as a function of latitude, longitude, and time of day, variations in the spatial distribution of the SO2, SO and S2 gases, which absorb strongly between 200 and 320 nm, and an un-identified ultraviolet {UV} absorber known to absorb strongly above 320 nm. Because the spatial distribution of all of the UV absorbers {named and un-named} is tied to the motion of the upper cloud, VCO plans to image the spatial distribution of the UV absorbers and their relationship with the cloud structure and the wind field, in order to derive the wind vectors at the cloud top {Rossow et al., 1990}. However, neither VEx nor VCO has the capability to obtain high spectral and spatial resolution spectroscopy of Venus upper clouds at 200-600 nm. The proposed HST observations will characterize and quantify the absorbers responsible for the cloud features recorded in the UV {200-600 nm} images to be obtained by the VCO/UVI and VEx/VIRTIS instruments, mapping the spatial distribution of these UV absorbers as function of the zonal cloud motion. Additionally, photodissociation of each of the identified UV absorbers is a key component of the system of reactions that leads to the formation of sulfur-oxides, the loss of atomic oxygen, and the subsequent formation of Venus H2SO4 clouds via the reaction of the sulfur-oxides with H2O. The density of H2O and OCS, the remaining atmospheric species that directly impact the rate of sulfur-oxide production and H2SO4 cloud formation within Venus atmosphere, will be obtained via ground-based and VEx/SOIR measurements. Thus, the proposed HST observations, when combined with VCO, VEx, and ground-based observations, will provide a complete picture of the latitudinal, longitudinal, time of day, and wind-driven variation of each of the key species involved in the sulfur-oxidation cycle. These results will be used to inform and develop models designed to i} investigate outstanding questions regarding the formation of Venus global sulfuric acid clouds and the abundance of oxygen in the atmosphere and ii} investigate the climatic evolution of Venus atmosphere.;
No associations
LandOfFree
Coordinated HST, Venus Express, and Venus Climate Orbiter Observations of Venus does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Coordinated HST, Venus Express, and Venus Climate Orbiter Observations of Venus, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Coordinated HST, Venus Express, and Venus Climate Orbiter Observations of Venus will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1786468