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3‐D Simulation of high‐latitude interaction regions: Comparison with Ulysses results
Author(s) -
Pizzo V. J.,
Gosling J. T.
Publication year - 1994
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/94gl01581
Subject(s) - physics , magnetohydrodynamic drive , solar wind , magnetohydrodynamics , latitude , heliosphere , interplanetary spaceflight , geophysics , coronal hole , interplanetary medium , low latitude , dipole , geology , astrophysics , coronal mass ejection , astronomy , plasma , quantum mechanics
A three‐dimensional (3‐D) magnetohydrodynamic (MHD) numerical model is used to simulate the global evolution of a steady, tilted‐dipole solar wind flow configuration similar to that prevalent in interplanetary space in 1993. Systematic latitudinal changes in the structure of a corotating interaction region (CIR) near 5 AU is shown to agree well with recent Ulysses observations. The abrupt disappearance of forward shocks and continued persistence of reverse shocks poleward of the latitude where Ulysses crossed the southern edge of the coronal streamer belt is explained as a natural consequence of the 3‐D flow geometry.