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The initial success of the Rigidly Rotating Magnetosphere (RRM) modelapplication to the B2Vp star sigma OriE by Townsend, Owocki & Groote (2005)triggered a renewed era of observational monitoring of this archetypal object.We utilize high-resolution spectropolarimetry and the magnetic Doppler imaging(MDI) technique to simultaneously determine the magnetic configuration, whichis predominately dipolar, with a polar strength Bd = 7.3-7.8 kG and a smallernon-axisymmetric quadrupolar contribution, as well as the surface distributionof abundance of He, Fe, C, and Si. We describe a revised RRM model that nowaccepts an arbitrary surface magnetic field configuration, with the fieldtopology from the MDI models used as input. The resulting synthetic Ha emissionand broadband photometric observations generally agree with observations,however, several features are poorly fit. To explore the possibility of aphotospheric contribution to the observed photometric variability, the MDIabundance maps were used to compute a synthetic photospheric light curve todetermine the effect of the surface inhomogeneities. Including the computedphotospheric brightness modulation fails to improve the agreement between theobserved and computed photometry. We conclude that the discrepancies cannot beexplained as an effect of inhomogeneous surface abundance. Analysis of the UVlight variability shows good agreement between observed variability andcomputed light curves, supporting the accuracy of the photospheric lightvariation calculation. We thus conclude that significant additional physics isnecessary for the RRM model to acceptably reproduce observations of not onlysigma Ori E, but also other similar stars with significant stellarwind-magnetic field interactions.

Revisiting the Rigidly Rotating Magnetosphere model for $\sigma$ Ori E - II. Magnetic Doppler imaging, arbitrary field RRM, and light variability