The Atmospheric Evolution Of Mars Indicated By C, N, Ar,
And H Isotopes
R. Hu, Jet Propulsion Laboratory, California Institute Of Technology, Pasadena, Ca, Usa
(Renyu.Hu@Jpl.Nasa.Gov), T. B. Thomas, Department Of Earth And Space Sciences, University Of Washington,
Seattle, Wa, Usa, E. L. Scheller, Division Of Geological And Planetary Sciences, California Institute Of Technology, Pasadena, Ca, Usa, D. J. Adams, Division Of Geological And Planetary Sciences, California Institute
Of Technology, Pasadena, Ca, Usa, B. L. Ehlmann, Division Of Geological And Planetary Sciences, California
Institute Of Technology, Pasadena, Ca, Usa, And Y. L. Yung, Division Of Geological And Planetary Sciences,
California Institute Of Technology, Pasadena, Ca, Usa.

Introduction:
The Initial Thickness, Evolution, And Loss Of The
Martian Atmosphere Have Been The Subject Of Much
Debate, As These Have Major Implications For The
Evolving Climate And Habitability Potential Of The Red
Planet. Recently, New Clues To This Problem Have
Been Found By Integrating Atmospheric And Geological Processes Into The Models Of The Isotope Budget
Of The Planet. The Isotopic Composition Of Carbon,
Nitrogen, Argon, And Hydrogen In Mars’S Atmosphere,
Together With The Extent Of Carbonates, Nitrates, And
Hydrated Minerals Found On The Planet, Provides Information About Its Atmospheric Evolution. We Have