Global Structure And Variability Of The Inner Hot
Oxygen Corona As Imaged By Emm/Emus
J. Deighan1 (Justin.Deighan@Lasp.Colorado.Edu), Michael Chaffin1, Krishnaprasad Chirakkil1,2, Hessa Rashid Almatroushi3, Robert J. Lillis4, Matthew O. Fillingim5, Scott England6, Sonal Jain1, Greg Holsclaw1,
Fatma Hussain Lootah7, Hoor Abdelrahman Almazmi8, F. G. Eparvier1, E. M. B. Thiemann1, P. C.
Chamberlin1
(1)Laboratory For Atmospheric And Space Physics, University Of Colorado Boulder, Boulder, Co, United
States,(2)Space And Planetary Science Center, Khalifa University Of Science Technology And Research, Abu
Dhabi, United Arab Emirates, (3)Mohammed Bin Rashid Space Center, Al Khawaneej, United Arab Emirates,
(4)Space Sciences Laboratory, University Of California Berkeley, Berkeley, Ca, United States, (5)University Of
California, Berkeley, Ca, United States, (6)Virginia Polytechnic Institute And State University, Aerospace And
Ocean Engineering, Blacksburg, Va, United States, (7)Mohammed Bin Rashid Space Centre, Dubai, United
Arab Emirates, (8)Uae Space Agency, Abu Dhabi, United Arab Emirates

Introduction:
The Hot Atomic Oxygen Corona Of Mars Is Composed Of A Hyper-Thermal Population (Energies Of
Order ~ 1 Ev) Resulting From Solar Euv Driven Photochemistry In The Planet’S Upper Atmosphere. A Fraction Of This Population Has Sufficient Velocity To Escape From The Planet, Representing A Mechanism For
Loss Of Atmosphere That Has Driven Planetary Evolution Over The History Of The Solar System. The Gravitationally Bound Portion Of The Corona Extends To Many
Planetary Radii, But Is Mostly Confined Within The First
Couple Radii Of The Planet. At Distances Within ~1/2
Martian Radius Above The Surface, The Structure Of