Observing Far-Ultraviolet Oxygen Aurorae In The Martian
Night-Side Atmosphere With Maven-Iuvs.
E. Lieb, Laboratory For Atmospheric And Space Physics (Emma.Lieb@Colorado.Edu), N. Schneider, Laboratory
For Atmospheric And Space Physics, J.C. Gerard, Lpap, Star Institute, University Of Liege, L. Soret, Lpap, Star
Institute, University Of Liege, S. Jain, Laboratory For Atmospheric And Space Physics.

Introduction
There Are At Least Three Types Of Aurorae On Mars; Discrete, Diffuse, And Proton. Discrete Aurorae Were First
Discovered By The Mars Express Spicam Instrument
And Are Further Supported By Maven Iuvs Observations. Figure 1 Panel A Shows A Typical Discrete Aurorae
Emission. These Aurorae Are Defined By Their Small,
Short-Lived Patches Of Emission Usually Related To The
Strong Crustal Field Region In The Southern Hemisphere
(Bertaux Et Al. (2005)). Diffuse Aurorae Were First Discovered By Maven Iuvs And Are Defined By Emission
That Spans Much Of The Martian Nightside Atmosphere
(Schneider Et Al. (2015); Jakosky Et Al. (2015); Schneider Et Al. (2018)). Figure 1, Panel B Shows An Example
Of A Diffuse Aurorae. These Emissions Are Caused By
Solar Energetic Particles (Seps), Specifically Electrons
And Protons Accelerated To Energies Of Roughly 100 Kev.
Lastly, Maven Iuvs Also Discovered Proton Aurorae