By J. vanVeeuwen
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Extra resources for Radio Pulsars
Although of a much lower signal-to-noise ratio, the shape of the phase envelope in each bin was consistent with that inferred with our preferred technique, which makes optimal use of all modulation power. Similarly, division of the observation into segments in time (which results in wider frequency bins and potentially also in reduced frequency drift in each segment) and examination of the phase relation in the peak bin of each segment also gave consistent results (regardless of the segment size).
Both shine normally for 98-99% of the time, to be occasionally interrupted for several seconds and then resume their normal emission. Both show similar changes in driftrate during nulls. It seems clear we see the same mechanism at work in these two pulsars. Yet for PSR B0809+74 we know the long nulls must be real, as the subpulse drift stops during these nulls (Chapter 2), while in PSR B0818−13 we never see long nulls. There we observe periods of intermittent emission and quietude, in groups about as long as the nulls in PSR B0809+74.
3%, with energies varying from 10 to 40% of the average pulse energy). For a pulse to have 10-40% of the normal energy, the null should start (stop) in the last (ﬁrst) 20% of the pulse windows, so within ± 2◦ . 5% of pulses, in of null are random, we would expect to see this happen in 360 good agreement with the values found above. If these low-energy pulses are really half-nulls, we would expect them to occur preferentially near null trains, as normal nulls do. We therefore calculated the mean distance to a null for both normal and low-energy pulses.