Solar wind forcing at Mercury: WSA‐ENLIL model results. Issue 1 (31st January 2013)

• Record Type: Journal Article
• Authors: Baker, Daniel N.; Poh, Gangkai; Odstrcil, Dusan; Arge, C. Nick; Benna, Mehdi; Johnson, Catherine L.; Korth, Haje; Gershman, Daniel J.; Ho, George C.; McClintock, William E.; Cassidy, Timothy A.; Merkel, Aimee; Raines, Jim M.; Schriver, David; Slavin, James A.; Solomon, Sean C.; Trávníček, Pavel M.; Winslow, Reka M.; Zurbuchen, Thomas H.
• Is Part Of: Journal of geophysical research. Volume 118:Issue 1(2013:Jan.)
• Page Start: 45
• Page End: 57
• Publication Date: 2013-01-31
• Subjects: MESSENGER; Magnetospheric physics -- Periodicals; Space environment -- Periodicals; Cosmic physics -- Periodicals; Planets -- Atmospheres -- Periodicals; Heliosphere (Astrophysics) -- Periodicals; Geophysics -- Periodicals; 523.01
• DOI: 10.1029/2012JA018064
• Languages: English
• ISSNs: 2169-9380

Abstract

Abstract : [1] Analysis and interpretation of observations from the MESSENGER spacecraft in orbit about Mercury require knowledge of solar wind "forcing" parameters. We have utilized the Wang‐Sheeley‐Arge (WSA)‐ENLIL solar wind modeling tool in order to calculate the values of interplanetary magnetic field (IMF) strength ( B ), solar wind velocity (V ) and density ( n ), ram pressure (~ nV 2 ), cross‐magnetosphere electric field (V × B ), Alfvén Mach number ( M A ), and other derived quantities of relevance for solar wind‐magnetosphere interactions. We have compared upstream MESSENGER IMF and solar wind measurements to see how well the ENLIL model results compare. Such parameters as solar wind dynamic pressure are key for determining the Mercury magnetopause standoff distance, for example. We also use the relatively high‐time‐resolutionB ‐field data from MESSENGER to estimate the strength of the product of the solar wind speed and southward IMF strength ( B s ) at Mercury. This product VB s is the electric field that drives many magnetospheric dynamical processes and can be compared with the occurrence of energetic particle bursts within the Mercury magnetosphere. This quantity also serves as input to the global magnetohydrodynamic and kinetic magnetosphere models that are being used to explore magnetospheric and exospheric processes at Mercury. Moreover, this modeling can help assess near‐real‐time magnetospheric behavior for MESSENGER or other mission analysis and/or ground‐based observational campaigns. We demonstrate that this solar wind forcing tool is a crucial step toward bringing heliospheric science expertise to bear on planetary exploration programs. Key Points: Correlation of model results with MESSENGER upstream measurements Use of solar wind model results to organize magnetospheric properties of Mercury Driving of Mercury magnetosphere