Comparing The My25 And My34 Global Dust Storms Using
The Ensemble Mars Atmosphere Reanalysis System (Emars)
N. Polek-Davis, Department Of Meteorology And Atmospheric Science, The Pennsylvania State University, University Park, Pa, Usa (Ntp5125@Psu.Edu), S. J. Greybush, Department Of Meteorology And Atmospheric Science, The Pennsylvania State University, University Park, Pa, Usa, R. J. Wilson, Space Science And Astrobiology Division, Nasa Ames Research Center, Moffett Field, Ca, Usa, R. P. Mcmichael, Department Of Meteorology And Atmospheric Science, The Pennsylvania State University, University Park, Pa, Usa, H. E. Gillespie,
Lunar And Planetary Institute, Universities Space Research Association, Houston, Tx, Usa.
Introduction: The Analysis Of Dust Storms Is Crucial Towards Understanding Martian Weather And Climate. Using The Ensemble Mars Atmosphere Reanalysis System (Emars; Greybush Et Al., 2019), This
Study Builds Upon That Understanding By Conducting A
Comparative Analysis Between Two Global Dust Storms.
While Regional Dust Storms Occur On Mars Every
Year, Every ~3-5 Years One Of These Storms Evolves
Into A Global Dust Storm (Gds). The My 25 Gds Began Around Ls 177˚ As Local Dust Storms Along The
Northwestern Rim Of Hellas Basin, Expanded To The
East And North, And Encircled The Planet By Ls 193˚
(Strausberg Et Al., 2005; Wolkenberg Et Al., 2020;
Wang Et Al., 2015). The My 34 Gds Began Around Ls
185˚ In Acidalia Around 10˚E, 60˚N, Expanded Westward And Equatorward, And Covered Mars By Ls 193˚
(Gillespie Et Al., 2020). In Both My25 And My34,
Common Features Include The Eastward Expansion Of
The Two Storms From Local Lifting Of The Tropics, And
The Initiation Of Multiple Dust-Lifting Centers That Were
Dynamically Active Throughout The Onset And Progression Of The Storm (Bertrand Et Al., 2020). Despite Similar Explosive Growth And Season Of Occurrence, The