Mars Atmospheric Thermal Structure During The 1st Year
Of Tgo Solar Occultation Measurements.
Miguel Angel LóPez-Valverde, (Valverde@Iaa.Es), B. Funke, A. Brines, A. Modak, A. Stolzenbach, F.
GonzáLez-Galindo, B. Hill, J. J. LóPez-Moreno, Instituto De Astrofı́Sica De Andalucia (Iaa/Csic), Granada, Spain
(Valverde@Iaa.Es), I. Thomas, L. Trompet, J. Erwin, Belgian Royal Institute For Space Aeronomy, Brussels, Belgium,
S. Aoki, University Of Tokyo, Japan, GeróNimo Villanueva, Nasa Goddard Space Flight Center, Usa, Giuliano Liuzzi, American University, Washington Dc, Usa, F. Forget, Laboratoire De Meteorologie Dynamique, Paris, France,
Giancarlo Bellucci, Institute For Space Astrophysics And Planetology, Italy, Manish Patel, Open University, Milton
Keynes, Uk, Bojan Ristic, Frank Daerden, Ann-Carine Vandaele, Belgian Royal Institute For Space Aeronomy,
Brussels, Belgium.

Introduction
The Detailed Variation Of Temperature And Density With
Altitude Is Of Paramount Importance To Characterize The
Atmospheric State And To Constrain The Chemistry, Radiation And Dynamics As A Whole. Only With An Accurate Description Of Vertical Variations With The Best
Possible Spatial And Resolution We Can Aim At Describing
The Key Exchanges Between Atmospheric Layers. These
Are Needed For Transport Of Radiatively Active Species,
For Energy Budget Modeling, Including Photochemistry,
Gravity Wave Propagation And Global Dynamics, And For
Atmospheric Escape Processes, To Mention A Few.