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Spatial Structure of Far Ultraviolet Martian Dayglow Observed by EMM-EMUS
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  • Scott L England,
  • Sonal Jain,
  • Justin Deighan,
  • Michael Scott Chaffin,
  • Gregory Holsclaw,
  • Joseph Scott Evans,
  • John Correira,
  • Matthew O Fillingim,
  • Robert James Lillis,
  • Hessa Almatroushi,
  • Fatma Hussain Lootah,
  • Hour Almazmi
Scott L England
Virginia Polytechnic Institute and State University

Corresponding Author:[email protected]

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Sonal Jain
LASP
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Justin Deighan
LASP
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Michael Scott Chaffin
LASP
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Gregory Holsclaw
University of Colorado Boulder
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Joseph Scott Evans
Computational Physics, Incorporated
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John Correira
Computational Physics, Inc.
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Matthew O Fillingim
University of California, Berkeley
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Robert James Lillis
University of California, Berkeley
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Hessa Almatroushi
Unknown
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Fatma Hussain Lootah
Mohammed Bin Rashid Space Centre
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Hour Almazmi
UAE Space Agency
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Abstract

Mars’ ultraviolet airglow has been used to study its upper atmosphere for over four decades. Identifying variations in emission features has provided information on composition, density and temperature. The Emirates Mars Ultraviolet Spectrometer onboard the Emirates Mars Mission observes Mars’ airglow at Far and Extreme UV wavelengths. Variations in disk emission features are studied, with a focus on O I 1304 Å, CO Fourth Positive Group and C I 1561 Å. All show variations with local time and emission angle as expected. Dawn-dusk asymmetry observed is attributed to local time differences in advection. Variations in the brightness of several dayglow features, including 1304 Å, with irregular shapes are noted in around 25% of the disk images. These display some local time and hemispheric asymmetry in their occurrence rates. Examination of their spatial structure, occurrence, and spectra suggests these are associated with variations in composition and photoelectron flux.