This cumbersome system has been replaced with a model-driven scheme in which vertical profiles are calculated for the full dayglow surface for the day of interest. These are combined into a three-dimensional data volume. Image analysis now requires only interpolation of pixel lines of sight through this modeled data volume, a much faster that allows data mining techniques to be used with UVI data. The next stage of development is to incorporate the 'pierce-point' approach of Strickland et al. This removes some of the slowest calculations from the data analysis process and should allow examination of even larger data sets.
Excellent agreement is seen.
Initial model runs by S. Bailey are essentially the same, which indicates that further analysis of the rocket data needs to be performed. This type of comparison is critical to understanding discrepancies between model and UVI observations and will be continued in the third year of funding. We are also developing techniques to automatically flag significant differences for more detailed investigation. These tools will enable searches of large quantities of UVI images for potential compositional changes as evidenced by changes in the 1356 dayglow. The principal task not yet addressed is the separate analysis of auroral images for composition information.