The solar wind interaction with Mars: Locations and shapes of the bow shock and the magnetic pile‐up boundary from the observations of the MAG/ER Experiment onboard Mars Global Surveyor

By D. Vignes, C. Mazelle, H. Rme, Mario H. Acuña, J. Connerney, R. Lin, D. Mitchell, P. Cloutier, D. Crider, N. F. Ness. 2000

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Structure, dynamics, and seasonal variability of the Mars‐solar wind interaction: MAVEN Solar Wind Ion Analyzer in‐flight performance and science results (2017, background): “suggest that the mean shock surface does not depend on solar cycle [Vignes et al., 2000], a conclusion which we should revisit once we have sufficient data.”
Three‐dimensional, multispecies, high spatial resolution MHD studies of the solar wind interaction with Mars (2004, background): “The calculated positions agree quite well with the average Mars Global Surveyor (MGS) results (shown by a dashed line) [Vignes et al., 2000].”
Strong plume fluxes at Mars observed by MAVEN: An important planetary ion escape channel (2015, background): “Plume fluxes are seen primarily in the northern MSE hemisphere above the MPB and gradually transition to tailward fluxes on the nightside without any significant boundary in between.”
Influence of the solar EUV flux on the Martian plasma environment (2005, unknown): “…the positions of both the bow shock and the MPB location are not significantly affected by the level of the solar EUV flux, at least with the spatial resolution of the present simulations, a conclusion in agreement with previous statistical analyses of bow shock crossings (Vignes et al., 2000).”