Journal article
Advancing Our Understanding of Martian Proton Aurora through a Coordinated Multi‐Model Comparison Campaign
Journal of geophysical research. Space physics, Vol.128(10), e2023JA031838
10/2023
DOI: 10.1029/2023JA031838
Abstract
Abstract Proton aurora are the most commonly observed yet least studied type of aurora at Mars. In order to better understand the physics and driving processes of Martian proton aurora, we undertake a multi‐model comparison campaign. We compare results from four different proton/hydrogen precipitation models with unique abilities to represent Martian proton aurora: Jolitz model (3‐D Monte Carlo), Kallio model (3‐D Monte Carlo), Bisikalo/Shematovich et al. model (1‐D kinetic Monte Carlo), and Gronoff et al. model (1‐D kinetic). This campaign is divided into two steps: an inter‐model comparison and a data‐model comparison. The inter‐model comparison entails modeling five different representative cases using similar constraints in order to better understand the capabilities and limitations of each of the models. Through this step we find that the two primary variables affecting proton aurora are the incident solar wind particle flux and velocity. In the data‐model comparison, we assess the robustness of each model based on its ability to reproduce a proton aurora observation. All models are able to effectively simulate the general shape of the data. Variations in modeled intensity and peak altitude can be attributed to differences in model capabilities/solving techniques and input assumptions ( e.g. , cross sections, 3‐D versus 1‐D solvers, and implementation of the relevant physics and processes). The good match between the observations and multiple models gives a measure of confidence that the appropriate physical processes and their associated parameters have been correctly identified and provides insight into the key physics that should be incorporated in future models.
Plain Language Summary The purpose of the present study is to gain a deeper understanding of the physics and driving processes of Martian proton aurora through a comparative modeling campaign. The models involved in this study have important similarities and differences, such as the dimensionality ( e.g ., 3‐D versus 1‐D), inputs, and relevant physics included. We separate the modeling campaign into two steps: a first step comparing the models with each other ( i.e. , model‐model comparison), and a second step comparing the simulated model results with data from a proton aurora observation ( i.e. , data‐model comparison) taken by the Imaging UltraViolet Spectrograph (IUVS) onboard the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft. We find that all of the models are able to effectively simulate the data in terms of shape and brightness range of the proton aurora observation. The results of this study inform our understanding of the primary influencing factors that cause variability in the Martian proton aurora profile, the effects of dynamically changing solar wind parameters on the coupled Mars‐Sun auroral system, and the physical processes/constraints that should be considered in future modeling attempts of this unique phenomenon. This article is protected by copyright. All rights reserved.
Key Points We undertake a multi‐model comparison campaign to gain a better understanding of the physics and driving processes of Martian proton aurora The incident solar wind particle flux and velocity are found to be the two most influential parameters affecting the proton aurora profile The models generally reproduce observations, with variations due to different model capabilities/solving techniques and input assumptions
Details
- Title: Subtitle
- Advancing Our Understanding of Martian Proton Aurora through a Coordinated Multi‐Model Comparison Campaign
- Creators
- Andréa C. G. Hughes - Goddard Space Flight CenterMichael Chaffin - University of Colorado BoulderEdwin Mierkiewicz - Embry–Riddle Aeronautical UniversityJustin Deighan - Laboratory for Atmospheric and Space PhysicsRebecca D. Jolitz - Laboratory for Atmospheric and Space PhysicsEsa Kallio - Aalto UniversityGuillaume Gronoff - Langley Research CenterValery Shematovich - Institute of Applied AstronomyDmitry Bisikalo - Institute of Astronomy of the Russian Academy of Sciences Moscow Russia, National Center for Physics and Mathematics Moscow RussiaJasper Halekas - University of IowaCyril Simon Wedlund - Space Research InstituteNicholas Schneider - Laboratory for Atmospheric and Space PhysicsBirgit Ritter - Royal Observatory of BelgiumZachary Girazian - University of IowaSonal Jain - University of Colorado BoulderJean‐Claude Gérard - Royal Observatory of BelgiumBradley Hegyi - Langley Research Center
- Resource Type
- Journal article
- Publication Details
- Journal of geophysical research. Space physics, Vol.128(10), e2023JA031838
- DOI
- 10.1029/2023JA031838
- ISSN
- 2169-9380
- eISSN
- 2169-9402
- Language
- English
- Electronic publication date
- 09/27/2023
- Date published
- 10/2023
- Academic Unit
- Physics and Astronomy
- Record Identifier
- 9984473950002771
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