Monitoring Ozone And Aerosol In The Martian Mesosphere
From Maven/Iuvs Stellar Occultation Observations Between
My 32 And 36.
A. S. Braude, F. Montmessin, L. Verdier, Z. Flimon, F. Lefevre, Latmos/Cnrs/Uvsq/Sorbonne/Paris-Saclay,
Guyancourt, France (Ashwin.Braude@Latmos.Ipsl.Fr), S. Gupta, S. K. Jain, N. M. Schneider, J. Deighan, Lasp, U.
Colorado, Boulder, Usa, F. Y. Jiang, R. Yelle, Lpl, U. Arizona, Tucson, Usa.

Introduction
In This Talk, We Will Present Vertically-Resolved Profiles
Of Ozone And Aerosol In The Mesosphere, As Retrieved
From Bimonthly Stellar Occultation Campaigns Carried
Out Between My 32 And 36 By The Imaging Ultraviolet Spectrograph (Iuvs) Instrument On Board The Mars
Atmosphere And Volatile Evolution Mission (Maven)
[1, 2]. Ozone Is Heavily Correlated With Other Products
Of The Photolysis Of Water Vapour In The Martian Atmosphere (Notably Ho X ) That Are More Difficult To Sense
Remotely (E.G. [3, 4]) But Which Play A Crucial Role In
The Stability Of Mars’ Co2 Atmosphere. Since Preliminary Data From My 32 And 33 Was Presented In [5] We
Have Refined The Process Of Filtering Out False Detections
Of Ozone In The Data, Which Has Allowed Us To Provide
More Reliable Vertical Profiles Not Only Of Ozone Number