The geometry of intermittent and magnetospheric state changes pulsars

Open Access

Fig. 9.

Relationship between η, R_η, and magnetic inclination angle, α, from Eq. (7). We derived η for selected pulsars with measured $\dot{ν}$ ${\dot {\nu }}$ ratios from SSW and from Young et al. (2012) for PSR B0823+26; we also derived the intermittent pulsars. The dashed curve is for R_η = 1.28.

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