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dc.contributor.authorHotan, Aidan
dc.contributor.authorBailes, M.
dc.contributor.authorOrd, Stephen
dc.date.accessioned2017-01-30T13:01:57Z
dc.date.available2017-01-30T13:01:57Z
dc.date.created2015-10-09T02:44:32Z
dc.date.issued2005
dc.identifier.citationHotan, A. and Bailes, M. and Ord, S. 2005. Geodetic precession in PSR J1141-6545. The Astrophysical Journal Letters. 624 (2): pp. 906-913.
dc.identifier.urihttp://hdl.handle.net/20.500.11937/27921
dc.identifier.doi10.1086/429270
dc.description.abstract

We present observations that show dramatic evolution of the mean pulse profile of the relativistic binary pulsar J1141--6545 over a period of five years. This is consistent with precession of the pulsar spin axis due to relativistic spin-orbit coupling. Observations made between 1999 and 2004 with a number of instruments at the Parkes radio telescope demonstrate a steady, secular evolution of the mean total intensity profile, which increases in width by more than 50 percent during the five year period. Analysis of the changing position angle of the linearly polarised component of the mean profile suggests that our line of sight is shifting closer to the core of the emission cone. We find that the slope of the position angle swing across the centre of the pulse steepens with time and use a simplified version of the rotating vector model to constrain the magnitude and direction of the change in our line of sight angle relative to the pulsar magnetic axis. The fact that we appear to be moving deeper into the emission cone is consistent with the non-detection of this pulsar in previous surveys.

dc.publisherInstitute of Physics Publishing Ltd.
dc.titleGeodetic precession in PSR J1141-6545
dc.typeJournal Article
dcterms.source.volume624
dcterms.source.number2
dcterms.source.startPage906
dcterms.source.endPage913
dcterms.source.issn2041-8205
dcterms.source.titleThe Astrophysical Journal Letters
curtin.accessStatusOpen access via publisher


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