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We report on the interannual variability of the atmospheric ice/dust cycle inthe Martian polar regions for Mars Years 28-30. We used CRISM emission phasefunction measurements to derive atmospheric dust optical depths and data fromthe MARCI instrument to derive atmospheric water ice optical depths. We haveused autocorrelation and cross correlation functions in order to quantify thedegree to which dust and ice are correlated throughout both polar regionsduring Mars Years 28-29. We find that in the south polar region, dust has thetendency to "self clear", demonstrated by negative autocorrelation around thecentral peak. This does not occur in the north polar region. In the south polarregion, dust and ice are temporally and spatially anti correlated. In the northpolar region, this relationship is reversed, however temporal correlation ofnorthern dust and ice clouds is weak - 6 times weaker than the anticorrelationin the south polar region. Our latitudinal autocorrelation functions allow usto put average spatial sizes of event cores and halos. Dust events in the southare largest, affecting almost the entire pole, whereas dust storms are smallerin the north. Ice clouds in north are similar in latitudinal extent to those inthe south (both have halos < 10{\deg}). Using cross-correlation functions ofwater ice and dust, we find that dust events temporally lag ice events by 35-80degrees of solar longitude in the north and south poles, which is likely due toseasonality of dust and ice events.

Correlations of atmospheric water ice and dust in the Martian Polar regions