Fig. 2
Polarisation degree as a function of a) the pulsar characteristic age τ; b) spin period Ps; c) spin period derivative Ṗs; d) spin-down power Ė; e) magnetic field at the surface Bs; and f) at the light cylinder BLC. The dotted lines show the best fit to the points with a linear function. The point in light grey deviates more than 1σ from the best fit.
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