SIMBAD references

We investigate properties of the emission 'on' and 'off' states in intermittent pulsars by modelling of the changes in spin-down rate between the two states, described by S_ R_ ={dot}ω_ on_/{dot}ω_ off_, as due to discrete changes of the spin-down torque in a magnetosphere of multiple states. In this model, each of the different spin-down rates corresponds to a unique magnetospheric state with a charge filling fraction, designated by the parameter y, and switching in the spin-down rate corresponds to a jump in the y value resulting in an abrupt change in S_R. We obtain trends of change in y_off as a function of S_R with and without presuming y_on and find that the magnetosphere is non-vacuum in the emission-off state as opposed to traditionally assumed. We consider two intermittent pulsars as example cases for the model. The identification of S_R up to six in our model implies that pulsars with large S_R is possible. We investigate the charge density, as indicated by y, in each emission state as a function of obliquity angle, α, for different S_R. Assuming a simple correlation between α and S_R, we estimate that changes in the latter as pulsar ages should be detectable. Our results suggest that more distinguishing features for intermittency are likely found in the emission-off state of an intermittent pulsar with small α.