Relating Dust Storm Morphology To Wave Dynamics.
J. M. Battalio, Dept. Of Earth And Planetary Sciences, Yale University, New Haven, Ct (Joseph.Battalio@Yale.Edu).

Introduction
Our Understanding Of Mars’S Weather And Dust Storms
Has Accelerated Over The Past Decades. Many Large Dust
Storms Originate In The Northern Hemisphere And Are
Caused By Traveling Baroclinic Waves; However, The Relationships Between Specific Dynamical Structures Within
These Waves And The Morphology Of Visible Dust Features
Remains Poorly Constrained. With The Development Of
Observation-Based Reanalysis Datasets, The Evolution Of
Dust Activity And Their Incipient Wave Structures Can Be
Better Determined. In Combination, These Datasets Can
Verify The Positions Of Air Masses, Cyclones, And Fronts
In Relation To Visible Structures In Dust Activity, Which
Are Needed To Validate Weather Models, And Will Further
Improve Our Understanding Of The Martian Dust Cycle.

Mars’S Major Dust Storms
Most Dust Storm Activity Is Confined Along The Edge Of