Spectroscopic Characterization Of Diatomic Molecules In The Martian
Atmosphere
R. Al Abdallah, Physics Department, Khalifa University, Abu-Dhabi (100059801@Ku.Ac.Ae) M. Khalil, Department Of Mechanical Engineering, Khalifa University, Abu-Dhabi, United Arab Emirates(100049371@Ku.Ac.Ae) , M. Gacesa, Physics Department, Space And Planetary Science Center, Khalifa
University, Abu-Dhabi, United Arab Emirates( Marko.Gacesa@Ku.Ac.Ae) , A. Al Ghaferi, Department Of Mechanical Engineering, Khalifa University, Abu-Dhabi, United Arab Emirates (Amal.Alghaferi@Ku.Ac.Ae) , N.
El-Kork, Physics Department, Space And Planetary Science Center, Khalifa University, Abu-Dhabi, United
Arab Emirates (Nayla.Elkork@Ku.Ac.Ae)

Introduction:
Over The Last Decades, Mar’S Climate Has Changed
Significantly From A Warmer, Water-Containing Planet
Into A Cold, Dry Global Desert. The Escape Of Atmospheric Gases To Space Likely Played A Role In This
Change. Jeans Escape Of Hydrogen, Photochemical
Escape Of Oxygen, And Acceleration Of Ions Above
Their Escape Velocities By The Interplanetary Magnetic
Fields And Solar Wind Plasma Constitute Pathways For
The Martian Atmospheric Loss.
Processes Involving Diatomic Molecules Also Play
An Important Role For This Depletion Process. For Example, It Was Proposed That The Collisions Of Hot Oxygen Atoms With Other Energetic Neutral Atoms (Enas)
Could Drive The Escape Of Light Atmospheric Gases,
Such As He [1], H2 [2], And Oh [3]. Our Goal Is To