000006548 001__ 6548
000006548 005__ 20240109102511.0
000006548 0247_ $$2DOI$$a10.1029/2023JA031838
000006548 037__ $$aSCART-2024-0005
000006548 100__ $$aHughes, A.C.G.
000006548 245__ $$aAdvancing Our Understanding of Martian Proton Aurora Through a Coordinated Multi-Model Comparison Campaign
000006548 260__ $$c2023
000006548 520__ $$aProton aurora are the most commonly observed yet least studied type of aurora at Mars. In order to better understand the physics and driving processes of Martian proton aurora, we undertake a multi-model comparison campaign. We compare results from four different proton/hydrogen precipitation models with unique abilities to represent Martian proton aurora: Jolitz model (3-D Monte Carlo), Kallio model (3-D Monte Carlo), Bisikalo/Shematovich et al. model (1-D kinetic Monte Carlo), and Gronoff et al. model (1-D kinetic). This campaign is divided into two steps: an inter-model comparison and a data-model comparison. The inter-model comparison entails modeling five different representative cases using similar constraints in order to better understand the capabilities and limitations of each of the models. Through this step we find that the two primary variables affecting proton aurora are the incident solar wind particle flux and velocity. In the data-model comparison, we assess the robustness of each model based on its ability to reproduce a proton aurora observation. All models are able to effectively simulate the general shape of the data. Variations in modeled intensity and peak altitude can be attributed to differences in model capabilities/solving techniques and input assumptions (e.g., cross sections, 3-D vs. 1-D solvers, and implementation of the relevant physics and processes). The good match between the observations and multiple models gives a measure of confidence that the appropriate physical processes and their associated parameters have been correctly identified and provides insight into the key physics that should be incorporated in future models.
000006548 594__ $$aNO
000006548 700__ $$aChaffin, M.
000006548 700__ $$aMierkiewicz, E.
000006548 700__ $$aDeighan, J.
000006548 700__ $$aJolitz, R.D.
000006548 700__ $$aKallio, E.
000006548 700__ $$aGronoff, G.
000006548 700__ $$aShematovich, V.
000006548 700__ $$aBisikalo, D.
000006548 700__ $$aHalekas, J.
000006548 700__ $$aWedlund, C.S.
000006548 700__ $$aSchneider, N
000006548 700__ $$aRitter, B.
000006548 700__ $$aGirazian, Z. 
000006548 700__ $$aJain, S.
000006548 700__ $$aGérard, J.-C.
000006548 700__ $$aHegyi, B.
000006548 773__ $$n10$$pJournal of Geophysical Research$$v128$$y2023
000006548 8560_ $$fbirgit.ritter@ksb-orb.be
000006548 905__ $$aaccepted to be published in
000006548 980__ $$aREFERD