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The non-collisional interaction between conducting obstacles and magnetizedplasma winds can be found in different scenarios, from the interactionoccurring between regions inside galaxy clusters to the interaction between thesolar wind and Mars, Venus, active comets or even the interaction between Titanand the Saturnian's magnetospheric flow. These objects generate, throughseveral current systems, perturbations in the streaming magnetic field leadingto its draping around the obstacle's effective conducting surface. Recentobservational results suggest that several properties associated with themagnetic field draping, such as the location of the polarity reversal layer ofthe induced magnetotail, are affected by variations in the conditions of thestreaming magnetic field. To improve our understanding of these phenomena, weperform a characterization of several magnetic field draping signatures byanalytically solving an ideal problem in which a perfectly conductingmagnetized plasma (with frozen-in magnetic field conditions) flows around aspherical body for various orientations of the streaming magnetic field. Inparticular, we compute the shift of the inverse polarity reversal layer as theorientation of the background magnetic field is changed.

Steady-State Magnetohydrodynamic Flow Around an Unmagnetized Conducting Sphere