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The coronal magnetic field is the primary driver of solar dynamic events.Linear and circular polarization signals of certain infrared coronal emissionlines contain information about the magnetic field, and to access thisinformation, either a forward or an inversion method must be used. We studythree coronal magnetic configurations that are applicable to polar-crownfilament cavities by doing forward calculations to produce syntheticpolarization data. We analyze these forward data to determine thedistinguishing characteristics of each model. We conclude that it is possibleto distinguish between cylindrical flux ropes, spheromak flux ropes, andsheared arcades using coronal polarization measurements. If one of these modelsis found to be consistent with observational measurements, it will meanpositive identification of the magnetic morphology that surrounds certainquiescent filaments, which will lead to a greater understanding of how theyform and why they erupt.

Polarimetric Properties of Flux-Ropes and Sheared Arcades in Coronal Prominence Cavities