Simulation Of The Atomic Deuterium Density And Escape At Mars And Comparison
With Maven/Iuvs Observations
J-Y. Chaufray, Latmos, Paris, France, F. Gonzalez-Galindo, Iaa, Csic, Granada, Spain, M. Vals, L. Rossi, F. Montmessin, F. Lefevre, F. Leblanc, R. Modolo, Latmos, Paris, France, F. Forget, E. Millour,
Lmd, Paris, France, G. Gilli, M. Lopez-Valverde, Iaa, Csic, Granada Spain, M. Mayyasi, Boston University, Ma, Usa

References:
Introduction:
The D/H Ratio Is A Key Parameter To Understand The
Atmospheric Evolution Of A Planet. On Mars A D/H ~
5 Times Larger Than The D/H Ratio Measured On Earth
Is Measured In Its Atmosphere. This Large Ratio Can Be
Explained By A Preferential Escape Of The Hydrogen
Compared To The Deuterium Due To Its Lower Mass.
However, While The Thermal Escape (Jeans Escape) Is
Strongly Mass Dependent Other Non-Thermal Processes
Are Less Mass Dependent And Would Impact The Time
Needed To Fractionate The Water From The Terrestrial
Value To The Current Value.
After The First Detections Of The Deuterium Lyman-Α
Emission From Earth (Bertaux Et Al. 1992, Krasnopolsky Et Al. 1998), The Mission Maven Performed