An Improved Model Of Water Ice Sublimation On Mars:
Validation At The Phoenix Landing Site
A. R. Khuller, School Of Earth And Space Exploration, Arizona State University, Tempe, Arizona, Usa
(Akhuller@Asu.Edu), G. D. Clow, Institute Of Arctic And Alpine Research, University Of Colorado, Boulder, Colorado, Usa.

Introduction:
While Numerous Authors [E.G., 1, 2] Have Modeled
The Sublimation Rate Of Exposed H2o Ice At The Surface
Of Mars, These Models Have Not Been Directly Validated
With In-Situ Data. Furthermore, Although Analog Studies Of Martian Ice Have Been Performed [3, 4], These
Studies Fail To Accurately Replicate Martian Ice Conditions In Terms Of Dust Content, Physical Scale And
Boundary Layer Atmospheric Conditions.
Here We Present Results From A One-Dimensional
Atmospheric Surface Layer Model That Calculates Turbulent Fluxes Over Planetary Surfaces To Predict The Sublimation Rates Of Ices (Co2, H2o, Ch4 Etc.). We Have
Validated Our Model Against Terrestrial And Martian Insitu Data. We Have Compared Our Results With The Predictions Of [1], Which Are Commonly Used By Martian
Ice Studies Today.
Methods: We Have Developed A Model Of The Atmospheric Surface Layer That Is Based On Previous Terrestrial/Martian Atmospheric Surface Layer Work [5, 6].
The Model Requires The Following Input Data: (1) Surface Pressure, (2) Surface Roughness, (3) Temperature
(At Two Heights), (4) Relative Humidity (At Two Heights)
And (5) Wind Speed. To Validate The Model, We Used