Journal article
Discrete Aurora at Mars: Dependence on Upstream Solar Wind Conditions
Journal of geophysical research. Space physics, Vol.127(4), e2021JA030238
04/2022
DOI: 10.1029/2021JA030238
Appears in UI Libraries Support Open Access
Abstract
Discrete aurora at Mars, characterized by their small spatial scale and tendency to form near strong crustal magnetic fields, are emissions produced by particle precipitation into the Martian upper atmosphere. Since 2014, Mars Atmosphere and Volatile EvolutioN's (MAVEN's) Imaging Ultraviolet Spectrograph (IUVS) has obtained a large collection of UV discrete aurora observations during its routine periapsis nightside limb scans. Initial analysis of these observations has shown that, near the strongest crustal magnetic fields in the southern hemisphere, the IUVS discrete aurora detection frequency is highly sensitive to the interplanetary magnetic field (IMF) clock angle. However, the role of other solar wind properties in controlling the discrete aurora detection frequency has not yet been determined. In this work, we use the IUVS discrete aurora observations, along with MAVEN observations of the upstream solar wind, to determine how the discrete aurora detection frequency varies with solar wind dynamic pressure, IMF strength, and IMF cone angle. We find that, outside of the strong crustal field region (SCFR) in the southern hemisphere, the aurora detection frequency is relatively insensitive to the IMF orientation, but significantly increases with solar wind dynamic pressure, and moderately increases with IMF strength. Interestingly however, although high solar wind dynamic pressures cause more aurora to form, they have little impact on the brightness of the auroral emissions. Alternatively, inside the SCFR, the detection frequency is only moderately dependent on the solar wind dynamic pressure, and is much more sensitive to the IMF clock and cone angles. In the SCFR, aurora are unlikely to occur when the IMF points near the radial or anti‐radial directions when the cone angle (arccos(Bx/|B|)) is less than 30° or between 120° and 150°. Together, these results provide the first comprehensive characterization of how upstream solar wind conditions affect the formation of discrete aurora at Mars.
Key Points
Outside the strong crustal field region, high solar wind pressures increase the aurora detection frequency but not the emission brightness
IMF orientation affects the aurora detection frequency more prominently near strong crustal fields
In the strong crustal field region, aurora are rare when the IMF points near the radial or anti‐radial directions
Details
- Title: Subtitle
- Discrete Aurora at Mars: Dependence on Upstream Solar Wind Conditions
- Creators
- Z. Girazian - University of Iowa, Physics and AstronomyN. M. Schneider - University of Colorado BoulderZ. Milby - Laboratory for Atmospheric and Space PhysicsX. Fang - University of Colorado BoulderJ. Halekas - University of Iowa, Physics and AstronomyT. Weber - University of Colorado BoulderS. K. Jain - University of Iowa, Psychological and Brain SciencesJ.‐C. Gérard - University of LiègeL. Soret - University of LiègeJ. Deighan - University of Colorado BoulderC. O. Lee - University of California, Berkeley
- Resource Type
- Journal article
- Publication Details
- Journal of geophysical research. Space physics, Vol.127(4), e2021JA030238
- DOI
- 10.1029/2021JA030238
- ISSN
- 2169-9380
- eISSN
- 2169-9402
- Publisher
- Wiley
- Number of pages
- 9
- Grant note
- European Space Agency (ESA) (4000121493) National Aeronautics and Space Administration (NASA) (MAVEN Mission; 80NSSC19K0562)
- Language
- English
- Date published
- 04/2022
- Academic Unit
- Physics and Astronomy
- Record Identifier
- 9984263558902771
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