Integrating In-Situ, Satellite, And Reanalysis Datasets
To Assess Temperature Profiles In The Martian Tropics
H. E. Gillespie, Universities Space Research Association (Usra)/Lunar And Planetary Institute (Lpi), Houston,
Tx (Hgillespie@Lpi.Usra.Edu), G. Martinez, Usra/Lpi, R. Hueso, University Of The Basque Country, Spain, A.
Munguira, University Of The Basque Country, Spain, E. Sebastián, Centro De Astrobiología, Spain, H.
Savijärvi, University Of Helsinki, Finland, A. Sánchez-Lavega, University Of The Basque Country, Spain, M.
Torre-Juárez, Jet Propulsion Laboratory, Usa, And J.A. Rodríguez-Manfredi, Centro De Astrobiología,
Spain

Introduction:
At The End Of The Night On Much Of Mars, Particularly Between Days With High Insolation, Near-Surface
Inversions Are Commonplace. The Low Thermal Inertia
Of Martian Soil Enables The Surface To Cool More
Rapidly At Night By Radiation Than The Atmosphere
Above. Observations By Mars Science Laboratory In
Gale Crater (Figure 1) And By Mini-Tes In Gusev
Crater And Near Endeavour Crater Show That Inversions Occur On The Vast Majority Of Nights In The
Martian Tropics [1–3]. However, Observations From
The Mars Environmental Dynamics Analyzer
(Meda) (Figure 2) Aboard Perseverance Show Inversions On About Half Of Nights In Jezero Crater