Journal
ASTROPHYSICAL JOURNAL
Volume 820, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/0004-637X/820/1/64
Keywords
pulsars: general; pulsars: individual (PSR J0835-4510); radiation mechanisms: non-thermal
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Funding
- Australian Government through its NCRIS program
- Australian Government through its RDSI program
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The mechanisms of emission and changes in rotation frequency (glitching) of the Vela pulsar (J0835-4510) are not well understood. Further insight into these mechanisms can be achieved by long-term studies of integrated pulse width, timing residuals, and bright-pulse rates. We have undertaken an intensive observing campaign of Vela and collected over 6000 hr of single-pulse data. The data shows that the pulse width changes with time, including marked jumps in width after micro-glitches (frequency changes). The abundance of bright pulses also changes after some micro-glitches, but not all. The secular changes in pulse width have three possible cyclic periods that match with X-ray periodicities of a helical jet that are interpreted as free precession.
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