The debate on the history of the Martian atmosphere continues without resolution. Much hinges on a satisfactory solution to the problem of what liquid was responsible for the extensive development of canyons, channels, fretted terrain, and similar features. The 1960s and 1970s saw much debate about the roles of various fluids, namely water or brine, liquid CO2, or H2O sources in CO2 clathrate (CC), or magma. The last was discounted long ago, CC is largely ignored, and the most recent look at CO2 was by ourselves, utilizing the phase diagrams for the CO2-H2O system. In this article, we will further investigate this dilemma.


    Access

    Access via TIB

    Check availability in my library


    Export, share and cite



    Title :

    CO2 and clathrate as past erosive agents on Mars


    Contributors:


    Publication date :

    1992-01-01


    Type of media :

    Conference paper


    Type of material :

    No indication


    Language :

    English




    Erosive Burning

    J. P. Renie / J. R. Osborn | AIAA | 1983


    EROSIVE BURNING REVISITED

    Landsbaum, E. M. / American Institute of Aeronautics and Astronautics / Society of Automotive Engineers et al. | British Library Conference Proceedings | 2003


    Erosive burning research

    STRAND, L. / YANG, L. / NGUYEN, M. et al. | AIAA | 1986


    Erosive Burning Revisited

    Landsbaum, Ellis | AIAA | 2003


    Mars Rovers, past and future

    Muirhead, Brian K. | NTRS | 2004