Impacts Of Heterogeneous Chemistry On Vertical Profiles
Of Martian Ozone.
M. A. J. Brown, School Of Physical Sciences, The Open University, Milton Keynes, U.K. (Megan.Brown@Open.Ac.Uk),
M. R. Patel, S. R. Lewis, J. A. Holmes, G. J. Sellers, P. M. Streeter, A. Bennaceaur, The Open University, Milton
Keynes, U.K., G. L. Villanueva, Planetary Systems Laboratory, Nasa Goddard Space Flight Center, Greenbelt, Md,
Usa, G. Liuzzi, Planetary Systems Laboratory, Nasa Goddard Space Flight Center, Greenbelt, Md, Usa, Department Of Physics, American University, Washington, Dc, Usa, A. C. Vandaele, Royal Belgian Institute For Space
Aeronomy (Bira-Iasb), Brussels, Belgium.

Background
Ozone (O3 ) Was First Detected In The Martian Atmosphere
In 1972 By Mariner 7 And Again By Mariner 10 (Barth
Et Al., 1973). Due To Its Chemical Sensitivity And Relatively Short Dayside Lifetime (2–3 Hours), It Is Often Used
As A Proxy For Other, Highly Reactive Species, Which Cannot Be Measured Directly With Remote Sensing (Clancy
And Nair, 1996). Such Chemical Species Include Hydroxyl Radicals (H, Oh, And Ho2 , Collectively Known
As Hox ), Which React With Ozone, And Participate In
Its Destruction. The Two Primary Destructive Pathways
Of Ozone Are From Uv Light (Via Photolysis) And Reactions With Hox Species (Clancy And Nair, 1996; LefèVre
Et Al., 2004). The Latter Can Cause A Set Of Chain Reactions Which Create More Hox Species And Lead, In Turn,
To Further Ozone Destruction. In Addition To Ozone Destruction, Hox Also Catalyse The Reaction Between Carbon
Monoxide (Co) And Molecular Oxygen (O), Recombining