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Marsh et al. detected radio and optical pulsations from the binary system ARScorpii (AR Sco). This system, with an orbital period of 3.56 h, is composed ofa cool, low-mass star and a white dwarf with a spin period of 1.95 min. Opticalobservations by Buckley et al. showed that the polarimetric emission from thewhite dwarf is strongly linearly polarised ( up to $\sim40\%$) withperiodically changing intensities. This periodic non-thermal emission isthought to be powered by the highly magnetised ($ 5 \times 10^{8} $ G) whitedwarf that is spinning down. The morphology of the polarisation signal, namelythe position angle plotted against the phase angle, is similar to that seen inmany radio pulsars. In this paper, we demonstrate that we can fit thetraditional pulsar rotating vector model to the optical position angle. We useda Markov-chain-Monte-Carlo technique to find the best fit for the modelyielding a magnetic inclination angle of $\alpha =(86.6^{+3.0}_{-2.8})^{\circ}$ and an observer angle of $\zeta =(60.5^{+5.3}_{-6.1})^{\circ}$. This modelling supports the scenario that thesynchrotron emission originates above the polar caps of the white dwarf pulsarand that the latter is an orthogonal rotator.

Modelling the polarisation signatures detected from the first white dwarf pulsar AR Sco